Author: "Menanteau F." / Topic: cosmology and nongalactic astrophysics (astro-ph.co) - Searchworks@Jio Institute Digital Library Search Results

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Start Over Author "Menanteau F." Topic cosmology and nongalactic astrophysics (astro-ph.co)

131 results on '"Menanteau F."'

1. Constraining the baryonic feedback with cosmic shear using the DES Year-3 small-scale measurements

Author: Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Nuclear Theory, High Energy Physics::Phenomenology, cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics Cosmology and Nongalactic Astrophysics, Space and Planetary Science, gravitational lensing weak, large-scale structure of Universe, cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package \texttt{Baccoemu} to accelerate the evaluation of the baryonic nonlinear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a $\sim 2 \sigma$ significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be $M_c > 10^{13.2} h^{-1} M_{\odot}$ (95\% C.L.). The best-fit baryonic suppression is $\sim 5\%$ at $k=1.0 {\rm Mpc}\ h^{-1}$ and $\sim 15\%$ at $k=5.0 {\rm Mpc} \ h^{-1}$. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments., Comment: 20 pages, 10 figures. DES Collaboration, Year-3 analysis
Published: 2022
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2. The DES view of the Eridanus supervoid and the CMB cold spot

Author: Kovács, A, Jeffrey, N, Gatti, M, Chang, C, Whiteway, L, Hamaus, N, Lahav, O, Pollina, G, Bacon, D, Kacprzak, T, Mawdsley, B, Nadathur, S, Zeurcher, D, García-Bellido, J, Alarcon, A, Amon, A, Bechtol, K, Bernstein, G M, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Cawthon, R, Chen, R, Choi, A, Cordero, J, Davis, C, Derose, J, Doux, C, Drlica-Wagner, A, Eckert, K, Elsner, F, Elvin-Poole, J, Everett, S, Ferté, A, Giannini, G, Gruen, D, Gruendl, R A, Harrison, I, Hartley, W G, Herner, K, Huff, E M, Huterer, D, Kuropatkin, N, Jarvis, M, Leget, P F, Maccrann, N, Mccullough, J, Muir, J, Myles, J, Navarro-Alsina, A, Pandey, S, Prat, J, Raveri, M, Rollins, R P, Ross, A J, Rykoff, E S, Sánchez, C, Secco, L F, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Troxel, M A, Tutusaus, I, Varga, T N, Yanny, B, Yin, B, Zhang, Y, Zuntz, J, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, D, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, Davis, T, Deundefined, Vicente, J, Desai, S, Diehl, H T, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, Gaztañaga, E, Gerdes, D, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S, Hollowood, D L, Honscheid, K, James, D, Kuehn, K, Lima, M, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Ogando, R, Paz-Chinchon, F, Pieres, A, Plazas, A A, Monroy, M Rodriguez, Romer, K, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, C-H, To, Weller, J, UAM. Departamento de Física Teórica, Instituto de Astrofísica de Canarias (IAC), Tenerife, Univer Sité de Paris, University College London, The Barcelona Institute of Science and Technology, University of Pennsylvania, University of Chicago, Univer Sity of Chica Go, Ludwig-Maximilians Univer- Sität München, University of Portsmouth, ETH Zurich, Universidad Autonoma de Madrid, Argonne National Laboratory, Stanford University, University of Wisconsin- Madison, Carnegie Mellon University, Laboratório Interinstitucional de E-Astronomia - LIneA, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, The Ohio State Univer- Sity, University of Manchester, University of California, Santa Cruz Institute for Particle Physics, Fermi National Accelerator Laboratory, The Ohio State University, California Institute of Technology, SLAC National Accelerator Laboratory, University of Oxford, University of Gene Va, University of Michigan, University of Cambridge, Perimeter Institute for Theoretical Physics, Univer Sidade Estadual de Campinas, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Institut D'Estudis Espacials de Catalunya (IEEC), CSIC), Max Planck Institute for Extraterrestrial Physics, University of Edinb Urgh, Universidade de São Paulo (USP), Universidade Estadual Paulista (UNESP), Institut D'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, IIT Hyderabad, University of Oslo, Univer Sity of Cambridge, Harvard and Smithsonian, Lowell Observatory, Macquarie University, Texas A&M Univer Sity, Princeton University, Institució Catalana de Recerca i Estudis Avan C Ats, Univer Sity of Sussex, University of Southampton, Oak Ridge National Labo- Ratory, Kovács, A, Jeffrey, N, Gatti, M, Chang, C, Whiteway, L, Hamaus, N, Lahav, O, Pollina, G, Bacon, D, Kacprzak, T, Mawdsley, B, Nadathur, S, Zeurcher, D, García-Bellido, J, Alarcon, A, Amon, A, Bechtol, K, Bernstein, G M, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Cawthon, R, Chen, R, Choi, A, Cordero, J, Davis, C, Derose, J, Doux, C, Drlica-Wagner, A, Eckert, K, Elsner, F, Elvin-Poole, J, Everett, S, Ferté, A, Giannini, G, Gruen, D, Gruendl, R A, Harrison, I, Hartley, W G, Herner, K, Huff, E M, Huterer, D, Kuropatkin, N, Jarvis, M, Leget, P F, Maccrann, N, Mccullough, J, Muir, J, Myles, J, Navarro-Alsina, A, Pandey, S, Prat, J, Raveri, M, Rollins, R P, Ross, A J, Rykoff, E S, Sánchez, C, Secco, L F, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Troxel, M A, Tutusaus, I, Varga, T N, Yanny, B, Yin, B, Zhang, Y, Zuntz, J, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, D, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, Davis, T, De&nbsp, Vicente, J, Desai, S, Diehl, H T, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, Gaztañaga, E, Gerdes, D, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S, Hollowood, D L, Honscheid, K, James, D, Kuehn, K, Lima, M, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Ogando, R, Paz-Chinchon, F, Pieres, A, Plazas, A A, Monroy, M Rodriguez, Romer, K, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, C-H, To, Weller, J, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Research Council, National Science Foundation (US), European Commission, and Agenzia Spaziale Italiana
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic Background Radiation, FOS: Physical sciences, Física, Astronomy and Astrophysics, cosmic background radiation, Surveys, gravitational lensing: weak, surveys, Space and Planetary Science, Weak [Gravitational Lensing], survey, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A. Kovács et al., The Cold Spot is a puzzling large-scale feature in the Cosmic Microwave Background temperature maps and its origin has been subject to active debate. As an important foreground structure at low redshift, the Eridanus supervoid was recently detected, but it was subsequently determined that, assuming the standard ΛCDM model, only about 10–20 per cent of the observed temperature depression can be accounted for via its Integrated Sachs–Wolfe imprint. However, R ≳ 100 h−1Mpc supervoids elsewhere in the sky have shown ISW imprints AISW ≈ 5.2 ± 1.6 times stronger than expected from ΛCDM (AISW = 1), which warrants further inspection. Using the Year-3 redMaGiC catalogue of luminous red galaxies from the Dark Energy Survey, here we confirm the detection of the Eridanus supervoid as a significant underdensity in the Cold Spot’s direction at z < 0.2. We also show, with S/N ≳ 5 significance, that the Eridanus supervoid appears as the most prominent large-scale underdensity in the dark matter mass maps that we reconstructed from DES Year-3 gravitational lensing data. While we report no significant anomalies, an interesting aspect is that the amplitude of the lensing signal from the Eridanus supervoid at the Cold Spot centre is about 30 per cent lower than expected from similar peaks found in N-body simulations based on the standard ΛCDM model with parameters Ωm = 0.279 and σ8 = 0.82. Overall, our results confirm the causal relation between these individually rare structures in the cosmic web and in the CMB, motivating more detailed future surveys in the Cold Spot region., AK has been supported by a Juan de la Cierva Incorporación fellowship with project number IJC2018-037730-I, and funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2021
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3. Mapping Variations of Redshift Distributions with Probability Integral Transforms

Author: Myles, J., Gruen, D., Amon, A., Alarcon, A., DeRose, J., Everett, S., Dodelson, S., Bernstein, G. M., Campos, A., Harrison, I., MacCrann, N., McCullough, J., Raveri, M., Sánchez, C., Troxel, M. A., Yin, B., Abbott, T. M. C., Allam, S., Alves, O., Andrade-Oliveira, F., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J. J., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vincenzi, M., Weaverdyck, N., DES Collaboration, Myles, J., Gruen, D., Amon, A., Alarcon, A., Derose, J., Everett, S., Dodelson, S., Bernstein, G. M., Campos, A., Harrison, I., Maccrann, N., Mccullough, J., Raveri, M., Sánchez, C., Troxel, M. A., Yin, B., Abbott, T. M. C., Allam, S., Alves, O., Andrade-Oliveira, F., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J. J., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plaza, Prat, J., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vincenzi, M., Weaverdyck, N., and Des, Collaboration
Subjects: Astrophysic, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, galaxies distances and redshift, FOS: Physical sciences, Astronomy and Astrophysics, gravitational lensing weak, methods numerical, galaxies distances and redshifts, Astrophysics, Cosmology and Nongalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a method for mapping variations between probability distribution functions and apply this method within the context of measuring galaxy redshift distributions from imaging survey data. This method, which we name PITPZ for the probability integral transformations it relies on, uses a difference in curves between distribution functions in an ensemble as a transformation to apply to another distribution function, thus transferring the variation in the ensemble to the latter distribution function. This procedure is broadly applicable to the problem of uncertainty propagation. In the context of redshift distributions, for example, the uncertainty contribution due to certain effects can be studied effectively only in simulations, thus necessitating a transfer of variation measured in simulations to the redshift distributions measured from data. We illustrate the use of PITPZ by using the method to propagate photometric calibration uncertainty to redshift distributions of the Dark Energy Survey Year 3 weak lensing source galaxies. For this test case, we find that PITPZ yields a lensing amplitude uncertainty estimate due to photometric calibration error within 1 per cent of the truth, compared to as much as a 30 per cent underestimate when using traditional methods.
Published: 2022

4. Velocity dispersions of clusters in the Dark Energy Survey Y3 redMaPPer catalogue

Author: A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, UAM. Departamento de Física Teórica, A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, Department of Energy (US), European Commission, European Research Council, Ministero dell'Istruzione, dell'Università e della Ricerca, Ministerio de Ciencia, Innovación y Universidades (España), Fundação para a Ciência e a Tecnologia (Portugal), Agencia Estatal de Investigación (España), National Science Foundation (US), Generalitat de Catalunya, and Ministerio de Economía y Competitividad (España)
Subjects: X-Rays: Galaxies: Clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Física, Astronomy and Astrophysics, galaxies: clusters: general, X-rays: galaxies: clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, clusters: general [galaxies], galaxies: clusters [X-rays], CLUSTERS, QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB, Galaxies: Clusters: General
Abstract: DES Collaboration: V. Wetzell et al., We measure the velocity dispersions of clusters of galaxies selected by the red-sequence Matched-filter Probabilistic Percolation (redMaPPer) algorithm in the first three years of data from the Dark Energy Survey (DES), allowing us to probe cluster selection and richness estimation, λ, in light of cluster dynamics. Our sample consists of 126 clusters with sufficient spectroscopy for individual velocity dispersion estimates. We examine the correlations between cluster velocity dispersion, richness, X-ray temperature, and luminosity, as well as central galaxy velocity offsets. The velocity dispersion–richness relation exhibits a bimodal distribution. The majority of clusters follow scaling relations between velocity dispersion, richness, and X-ray properties similar to those found for previous samples; however, there is a significant population of clusters with velocity dispersions that are high for their richness. These clusters account for roughly 22 per cent of the λ < 70 systems in our sample, but more than half (55 per cent) of λ < 70 clusters at z > 0.5. A couple of these systems are hot and X-ray bright as expected for massive clusters with richnesses that appear to have been underestimated, but most appear to have high velocity dispersions for their X-ray properties likely due to line-of-sight structure. These results suggest that projection effects contribute significantly to redMaPPer selection, particularly at higher redshifts and lower richnesses. The redMaPPer determined richnesses for the velocity dispersion outliers are consistent with their X-ray properties, but several are X-ray undetected and deeper data are needed to understand their nature., This work was supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Numbers DE-SC0010107 and A00-1465-001. AS is supported by the ERC-StG ‘ClustersXCosmo’ grant agreement 716762, by the FARE-MIUR grant ’ClustersXEuclid’ R165SBKTMA, and by INFN InDark Grant. PTPV was supported by Fundação para a Ciência e a Tecnologia (FCT) through research grants UIDB/04434/2020andUIDP/04434/2020. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the University of Illinois at Urbana-Champaign - National Center for Supercomputing Applications, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California, Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas – Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians-Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This study is based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the EU Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022
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5. The Intrinsic Alignment of Red Galaxies in DES Y1 redMaPPer Galaxy Clusters

Author: Zhou, C., Tong, A., Troxel, M. A., Blazek, J., Lin, C., Bacon, D., Bleem, L., Rosell, A. Carnero, Chang, C., Costanzi, M., DeRose, J., Dietrich, J. P., Drlica-Wagner, A., Gruen, D., Gruendl, R. A., Hoyle, B., Jarvis, M., MacCrann, N., Mawdsley, B., McClintock, T., Melchior, P., Prat, J., Pujol, A., Rozo, E., Rykoff, E. S., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Tucker, D. L., Varga, T. N., Yanny, B., Zhang, Y., Zuntz, J., Alves, O., Amon, A., Bertin, E., Brooks, D., Burke, D. L., Kind, M. Carrasco, da Costa, L. N., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Raveri, M., Romer, A. K., Sanchez, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Weaverdyck, N., Weller, J., and Wiseman, P.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Clusters of galaxies are sensitive to the most nonlinear peaks in the cosmic density field. The weak gravitational lensing of background galaxies by clusters can allow us to infer their masses. However, galaxies associated with the local environment of the cluster can also be intrinsically aligned due to the local tidal gradient, contaminating any cosmology derived from the lensing signal. We measure this intrinsic alignment in Dark Energy Survey (DES) Year 1 redMaPPer clusters. We find evidence of a non-zero mean radial alignment of galaxies within clusters between redshift 0.1-0.7. We find a significant systematic in the measured ellipticities of cluster satellite galaxies that we attribute to the central galaxy flux and other intracluster light. We attempt to correct this signal, and fit a simple model for intrinsic alignment amplitude ($A_{\textrm{IA}}$) to the measurement, finding $A_{\textrm{IA}}=0.15\pm 0.04$, when excluding data near the edge of the cluster. We find a significantly stronger alignment of the central galaxy with the cluster dark matter halo at low redshift and with higher richness and central galaxy absolute magnitude (proxies for cluster mass). This is an important demonstration of the ability of large photometric data sets like DES to provide direct constraints on the intrinsic alignment of galaxies within clusters. These measurements can inform improvements to small-scale modeling and simulation of the intrinsic alignment of galaxies to help improve the separation of the intrinsic alignment signal in weak lensing studies., 14 pages, 13 figures
Published: 2023

6. Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies

Author: Chen, R, Scolnic, D, Rozo, E, Rykoff, ES, Popovic, B, Kessler, R, Vincenzi, M, Davis, TM, Armstrong, P, Brout, D, Galbany, L, Kelsey, L, Lidman, C, Möller, A, Rose, B, Sako, M, Sullivan, M, Taylor, G, Wiseman, P, Asorey, J, Carr, A, Conselice, C, Kuehn, K, Lewis, GF, Macaulay, E, Rodriguez-Monroy, M, Tucker, BE, Abbott, TMC, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bacon, D, Bertin, E, Bocquet, S, Brooks, D, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Cawthon, R, Costanzi, M, Da Costa, LN, Pereira, MES, Desai, S, Diehl, HT, Doel, P, Everett, S, Ferrero, I, Flaugher, B, Friedel, D, Frieman, J, García-Bellido, J, Gatti, M, Gaztanaga, E, Gruen, D, Hinton, Hollowood, DL, Honscheid, K, James, DJ, Lahav, O, Lima, M, March, M, Menanteau, F, Miquel, R, Morgan, R, Palmese, A, Paz-Chinchón, F, Pieres, A, Plazas Malagón, AA, Prat, J, Romer, AK, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Tarle, G, Thomas, D, To, C, Tucker, DL, Varga, TN, Department of Energy (US), National Aeronautics and Space Administration (US), National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, European Research Council, Chen, R., Scolnic, D., Rozo, E., Rykoff, E. S., Popovic, B., Kessler, R., Vincenzi, M., Davis, T. M., Armstrong, P., Brout, D., Galbany, L., Kelsey, L., Lidman, C., Möller, A., Rose, B., Sako, M., Sullivan, M., Taylor, G., Wiseman, P., Asorey, J., Carr, A., Conselice, C., Kuehn, K., Lewis, G. F., Macaulay, E., Rodriguez-Monroy, M., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gruen, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Lahav, O., Lima, M., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Prat, J., Romer, A. K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Chen, R [0000-0003-3917-0966], Rykoff, ES [0000-0001-9376-3135], Popovic, B [0000-0002-8012-6978], Kessler, R [0000-0003-3221-0419], Davis, TM [0000-0002-4213-8783], Brout, D [0000-0001-5201-8374], Galbany, L [0000-0002-1296-6887], Lidman, C [0000-0003-1731-0497], Sako, M [0000-0003-2764-7093], Sullivan, M [0000-0001-9053-4820], Carr, A [0000-0003-4074-5659], Conselice, C [0000-0003-1949-7638], Kuehn, K [0000-0003-0120-0808], Lewis, GF [0000-0003-3081-9319], Tucker, BE [0000-0002-4283-5159], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Bocquet, S [0000-0002-4900-805X], Brooks, D [0000-0002-8458-5047], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], Desai, S [0000-0002-0466-3288], Diehl, HT [0000-0002-8357-7467], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Gruen, D [0000-0003-3270-7644], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Romer, AK [0000-0002-9328-879X], Roodman, A [0000-0001-5326-3486], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Smith, M [0000-0002-3321-1432], Soares-Santos, M [0000-0001-6082-8529], Tarle, G [0000-0003-1704-0781], Thomas, D [0000-0002-6325-5671], Tucker, DL [0000-0001-7211-5729], and Apollo - University of Cambridge Repository
Subjects: Type Ia supernovae, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, COSMOLOGIA, 5109 Space Sciences, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 51 Physical Sciences, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: Chen et al., Current and future cosmological analyses with Type Ia supernovae (SNe Ia) face three critical challenges: (i) measuring the redshifts from the SNe or their host galaxies; (ii) classifying the SNe without spectra; and (iii) accounting for correlations between the properties of SNe Ia and their host galaxies. We present here a novel approach that addresses each of these challenges. In the context of the Dark Energy Survey (DES), we analyze an SN Ia sample with host galaxies in the redMaGiC galaxy catalog, a selection of luminous red galaxies. redMaGiC photo-z estimates are expected to be accurate to σΔz/(1+z) ∼ 0.02. The DES-5YR photometrically classified SN Ia sample contains approximately 1600 SNe, and 125 of these SNe are in redMaGiC galaxies. We demonstrate that redMaGiC galaxies almost exclusively host SNe Ia, reducing concerns relating to classification uncertainties. With this subsample, we find similar Hubble scatter (to within ∼0.01 mag) using photometric redshifts in place of spectroscopic redshifts. With detailed simulations, we show that the bias due to using redMaGiC photo-zs on the measurement of the dark energy equation of state w is up to Δw ∼ 0.01–0.02. With real data, we measure a difference in w when using the redMaGiC photo-zs versus the spec-zs of Δw = 0.005. Finally, we discuss how SNe in redMaGiC galaxies appear to comprise a more standardizable population, due to a weaker relation between color and luminosity (β) compared to the DES-3YR population by ∼5σ. These results establish the feasibility of performing redMaGiC SN cosmology with photometric survey data in the absence of spectroscopic data., D.S. is supported by DOE grant No. DE-SC0010007 and the David and Lucile Packard Foundation. D.S. is supported in part by NASA under Contract No. NNG17PX03C, issued through the WFIRST Science Investigation Teams Programme. E. Rozo is supported by NSF grant No. 2009401. E. Rozo is further supported by DOE grant No. DE-SC0009913 and by a Cottrell Scholar award. L.K. thanks the UKRI Future Leaders Fellowship for support through grant No. MR/T01881X/1. L.G. acknowledges financial support from the Spanish Ministry of Science and Innovation (MCIN) under the 2019 Ramón y Cajal program RYC2019-027683-I and from the Spanish MCIN project HOSTFLOWS PID2020-115253GA-I00. This paper has gone through internal review by the DES collaboration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS's NOIRLab, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grant Nos. ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007–2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2022

7. Dark Energy Survey Year 3 results: Cosmology from combined galaxy clustering and lensing validation on cosmological simulations

Author: DeRose, J., Wechsler, R. H., Becker, M. R., Rykoff, E. S., Pandey, S., MacCrann, N., Amon, A., Myles, J., Krause, E., Gruen, D., Jain, B., Troxel, M. A., Prat, J., Alarcon, A., Sanchez, C., Blazek, J., Crocce, M., Giannini, G., Gatti, M., Bernstein, G. M., Zuntz, J., Dodelson, S., Fang, X., Friedrich, O., Secco, L. F., Elvin-Poole, J., Porredon, A., Everett, S., Choi, A., Harrison, I., Cordero, J., Rodriguez-Monroy, M., McCullough, J., Cawthon, R., Chen, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Gruendl, R. A., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Raveri, M., Rosenfeld, R., Ross, A. J., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Yin, B., Zhang, Y., Fosalba, P., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Ferte, A., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., UAM. Departamento de Física Teórica, A DeRose, J., Wechsler, R. H., Becker, M. R., Rykoff, E. S., Pandey, S., Maccrann, N., Amon, A., Myles, J., Krause, E., Gruen, D., Jain, B., Troxel, M. A., Prat, J., Alarcon, A., Sánchez, C., Blazek, J., Crocce, M., Giannini, G., Gatti, M., Bernstein, G. M., Zuntz, J., Dodelson, S., Fang, X., Friedrich, O., Secco, L. F., Elvin-Poole, J., Porredon, A., Everett, S., Choi, A., Harrison, I., Cordero, J., Rodriguez-Monroy, M., Mccullough, J., Cawthon, R., Chen, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Gruendl, R. A., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Raveri, M., Rosenfeld, R., Ross, A. J., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Yin, B., Zhang, Y., Fosalba, P., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plaza, Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Commission, European Research Council, and Generalitat de Catalunya
Subjects: data release, Gravitational Lensing, model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), sky surveys, strophysics, FOS: Physical sciences, Física, Astrophysics::Cosmology and Extragalactic Astrophysics, oscillation spectroscopic survey, calibration, des, Dark Energy, Cosmology and Nongalactic Astrophysics, strophysic, challenge, impact, astro-ph.CO, Weak, redshift distributions, sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: J. DeRose et al., We present a validation of the Dark Energy Survey Year 3 (DES Y3) 3×2-point analysis choices by testing them on Buzzard2.0, a new suite of cosmological simulations that is tailored for the testing and validation of combined galaxy clustering and weak-lensing analyses. We show that the buzzard2.0 simulations accurately reproduce many important aspects of the DES Y3 data, including photometric redshift and magnitude distributions, and the relevant set of two-point clustering and weak-lensing statistics. We then show that our model for the 3×2-point data vector is accurate enough to recover the true cosmology in simulated surveys assuming the true redshift distributions for our source and lens samples, demonstrating robustness to uncertainties in the modeling of the nonlinear matter power spectrum, nonlinear galaxy bias, and higher-order lensing corrections. Additionally, we demonstrate for the first time that our photometric redshift calibration methodology, including information from photometry, spectroscopy, clustering cross-correlations, and galaxy–galaxy lensing ratios, is accurate enough to recover the true cosmology in simulated surveys in the presence of realistic photometric redshift uncertainties., J. D. is supported by the Chamberlain fellowship at Lawrence Berkeley National Laboratory. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under Contract No. DE-AC02-05CH11231. We would like to thank Stanford University and the Stanford Research Computing Center for providing computational resources and support that contributed to these research results. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DESBrazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the LudwigMaximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This paper is based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST1138766andNo.AST-1536171.The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I.F. A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants No. 240672, No.291329,andNo.306478.Weacknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia(INCT)doe-Universo(CNPqGrantNo.465376/ 2014-2). This manuscript has been authored by Fermi Research Alliance, LLC, under Contract No. DE-AC0207CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022
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8. Mapping gas around massive galaxies: cross-correlation of DES Y3 galaxies and Compton-$y$-maps from SPT and Planck

Author: Sánchez, J., Omori, Y., Chang, C., Bleem, L. E., Crawford, T., Drlica-Wagner, A., Raghunathan, S., Zacharegkas, G., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Avila, S., Baxter, E., Bechtol, K., Benson, B. A., Bernstein, G. M., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Campos, A., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C. L., Chen, A., Choi, A., Chown, R., Costanzi, M., Crites, A. T., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Haan, T., De Vicente, J., DeRose, J., Desai, S., Diehl, H. T., Dobbs, M. A., Dodelson, S., Doel, P., Elvin-Poole, J., Everett, W., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gatti, M., George, E. M., Gerdes, D. W., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Hinton, S. R., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., James, D. J., Knox, L., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A. T., Luong-Van, D., MacCrann, N., Marshall, J. L., McCullough, J., McMahon, J. J., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mocanu, L., Mohr, J. J., Muir, J., Myles, J., Natoli, T., Padin, S., Palmese, A., Pandey, S., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Pryke, C., Raveri, M., Reichardt, C. L., Rodriguez-Monroy, M., Ross, A. J., Ruhl, J. E., Rykoff, E., Sánchez, C., Sanchez, E., Scarpine, V., Schaffer, K. K., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Smith, M., Soares-Santos, M., Staniszewski, Z., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vieira, J. D., Vincenzi, M., Weaverdyck, N., Williamson, R., Yanny, B., Yin, B., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), CEA/DSM Centre de Saclay (CEA/DSM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), DES, and SPT
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology: observations, FOS: Physical sciences, galaxies: structure, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We cross-correlate positions of galaxies measured in data from the first three years of the Dark Energy Survey with Compton-$y$-maps generated using data from the South Pole Telescope (SPT) and the {\it Planck} mission. We model this cross-correlation measurement together with the galaxy auto-correlation to constrain the distribution of gas in the Universe. We measure the hydrostatic mass bias or, equivalently, the mean halo bias-weighted electron pressure $\langle b_{h}P_{e}\rangle$, using large-scale information. We find $\langle b_{h}P_{e}\rangle$ to be $[0.16^{+0.03}_{-0.04},0.28^{+0.04}_{-0.05},0.45^{+0.06}_{-0.10},0.54^{+0.08}_{-0.07},0.61^{+0.08}_{-0.06},0.63^{+0.07}_{-0.08}]$ meV cm$^{-3}$ at redshifts $z \sim [0.30, 0.46, 0.62,0.77, 0.89, 0.97]$. These values are consistent with previous work where measurements exist in the redshift range. We also constrain the mean gas profile using small-scale information, enabled by the high-resolution of the SPT data. We compare our measurements to different parametrized profiles based on the cosmo-OWLS hydrodynamical simulations. We find that our data are consistent with the simulation that assumes an AGN heating temperature of $10^{8.5}$K but are incompatible with the model that assumes an AGN heating temperature of $10^{8.0}$K. These comparisons indicate that the data prefer a higher value of electron pressure than the simulations within $r_{500c}$ of the galaxies' halos., Comment: 20 pages, 9 figures. Submitted to MNRAS
Published: 2023
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9. The Dark Energy Survey Year 3 and eBOSS: constraining galaxy intrinsic alignments across luminosity and colour space

Author: Samuroff, S., Mandelbaum, R., Blazek, J., Campos, A., MacCrann, N., Zacharegkas, G., Amon, A., Prat, J., Singh, S., Elvin-Poole, J., Ross, A. J., Alarcon, A., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Choi, A., Crocce, M., Davis, C., DeRose, J., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Everett, S., Ferté, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Herner, K., Huff, E. M., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., McCullough, J., Myles, J., Navarro-Alsina, A., Pandey, S., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rossi, G., Rykoff, E. S., Sánchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M. A., Tutusaus, I., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Aguena, J. Zuntz M., Alves, O., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Newman, J., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Sanchez, E., Scarpine, V., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., and To, C.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present direct constraints on galaxy intrinsic alignments using the Dark Energy Survey Year 3 (DES Y3), the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) and its precursor, the Baryon Oscillation Spectroscopic Survey (BOSS). Our measurements incorporate photometric red sequence (redMaGiC) galaxies from DES with median redshift $z\sim0.2-1.0$, luminous red galaxies (LRGs) from eBOSS at $z\sim0.8$, and also a SDSS-III BOSS CMASS sample at $z\sim0.5$. We measure two point intrinsic alignment correlations, which we fit using a model that includes lensing, magnification and photometric redshift error. Fitting on scales $6, Comment: Submitted to MNRAS; 22 pages, 11 figures
Published: 2022

10. The Dark Energy Survey Year 3 high redshift sample: Selection, characterization and analysis of galaxy clustering

Author: Sánchez, C., Alarcon, A., Bernstein, G. M., Sanchez, J., Pandey, S., Raveri, M., Prat, J., Weaverdyck, N., Sevilla-Noarbe, I., Chang, C., Baxter, E., Omori, Y., Jain, B., Alves, O., Amon, A., Bechtol, K., Becker, M. R., Blazek, J., Choi, A., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Crocce, M., Cross, D., Derose, J., Diehl, H. T., Dodelson, S., Drlicawagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Xiao Fang, Fosalba, P., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Maccrann, N., Mccullough, J., Myles, J., Krause, E., Porredon, A., Rodriguezmonroy, M., Rykoff, E. S., Secco, L. F., Sheldon, E., Troxel, M. A., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., Desai, S., Doel, P., Doux, C., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gutierrez, G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and HEP, INSPIRE
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The fiducial cosmological analyses of imaging galaxy surveys like the Dark Energy Survey (DES) typically probe the Universe at redshifts $z < 1$. This is mainly because of the limited depth of these surveys, and also because such analyses rely heavily on galaxy lensing, which is more efficient at low redshifts. In this work we present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around $z \sim 0.9$, $1.2$ and $1.5$, which significantly extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions. The analysis of galaxy clustering measurements, with a total signal-to-noise $S/N \sim 70$ after scale cuts, yields robust cosmological constraints on a combination of the fraction of matter in the Universe $\Omega_m$ and the Hubble parameter $h$, $\Omega_m h = 0.195^{+0.023}_{-0.018}$, and 2-3% measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, $b \sigma_8$. A companion paper $\textit{(in preparation)}$ will present the cross-correlations of these high-$z$ samples with CMB lensing from Planck and SPT, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work., Comment: 28 pages, 25 figures. To be submitted to MNRAS. Comments welcome
Published: 2022

11. The maxPSZ catalogue of Planck clusters over the DES region

Author: Hernández-Lang, D., Klein, M., Mohr, J. J., Grandis, S., Melin, J. -B., Tarrío, P., Arnaud, M., Pratt, G. W., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., and Weaverdyck, N.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first systematic follow-up of Planck Sunyaev-Zeldovich effect (SZE) selected candidates down to signal-to-noise (S/N) of 3 over the 5000 deg$^2$ covered by the Dark Energy Survey. Using the MCMF cluster confirmation algorithm, we identify optical counterparts, determine photometric redshifts and richnesses and assign a parameter, $f_{\rm cont}$, that reflects the probability that each SZE-optical pairing represents a random superposition of physically unassociated systems rather than a real cluster. The new maxPSZ cluster catalogue consists of 853 MCMF confirmed clusters and has a purity of 90%. We present the properties of subsamples of the maxPSZ catalogue that have purities ranging from 90% to 97.5%, depending on the adopted $f_{\rm cont}$ threshold. Halo mass estimates $M_{500}$, redshifts, richnesses, and optical centers are presented for all maxPSZ clusters. The maxPSZ catalogue adds 589 previously unknown Planck identified clusters over the DES footprint and provides redshifts for an additional 50 previously published Planck selected clusters with S/N>4.5. Using the subsample with spectroscopic redshifts, we demonstrate excellent cluster photo-$z$ performance with an RMS scatter in $Δz/(1+z)$ of 0.47%. Our MCMF based analysis allows us to infer the contamination fraction of the initial S/N>3 Planck selected candidate list, which is ~50%. We present a method of estimating the completeness of the maxPSZ cluster sample. In comparison to the previously published Planck cluster catalogues. this new S/N>3 MCMF confirmed cluster catalogue populates the lower mass regime at all redshifts and includes clusters up to z$\sim$1.3., 20 pages, 5 Appendices, 17 figures, submitted to MNRAS
Published: 2022

12. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

Author: Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Carnero Rosell, A., Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Carrasco Kind, M., Chintalapati, P., Cordero, J., Derose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., Maccrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Des, Collaboration, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Generalitat de Catalunya, European Research Council, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Carnero Rosell, A., Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Carrasco Kind, M., Chintalapati, P., Cordero, J., Derose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., Maccrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Des, Collaboration, HEP, INSPIRE, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: luminous red galaxies, data release, pau survey, Cosmology and Nongalactic Astrophysics (astro-ph.CO), roman-space-telescope, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, oscillation spectroscopic survey, Astrophysic, Cosmology and Nongalactic Astrophysics, internal consistency, digital sky survey, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], photometric data set, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Porredon et al., The cosmological information extracted from photometric surveys is most robust when multiple probes of the large scale structure of the Universe are used. Two of the most sensitive probes are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the way galaxies trace matter (the galaxy bias factor). The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000deg2 of the Dark Energy Survey’s first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies, especially selected to optimize such combination, and 100 million background shapes. We consider two flat cosmological models, the Standard Model with dark energy and cold dark matter (ΛCDM ) a variation with a free parameter for the dark energy equation of state (wCDM). Both models are marginalized over 25 astrophysical and systematic nuisance parameters. In ΛCDM we obtain for the matter density Ωm=0.320+0.041−0.034 and for the clustering amplitude S8≡σ8(Ωm/0.3)0.5=0.778+0.037−0.031, at 68% C.L. The latter is only 1σ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In wCDM we find Ωm=0.32+0.044−0.046, S8=0.777+0.049−0.051 and dark energy equation of state w=−1.031+0.218−0.379. We find that including smaller scales, while marginalizing over nonlinear galaxy bias, improves the constraining power in the Ωm−S8 plane by 31% and in the Ωm−w plane by 41% while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3×2pt)., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management systemis supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds fromthe European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a nonexclusive paid-up irrevocable world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. Computations were made on the supercomputer Guillimin from McGill University, managed by Calcul Quebec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), the ministere de l’Économie, de la science et de l’innovation du Quebec (MESI) and the Fonds de recherche du Quebec-Nature et technologies (FRQ-NT). This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Grants No. OCI-0725070 and No. ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This research used resources of the Ohio Supercomputer Center (OSC) [117] and of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231.
Published: 2022

13. A galaxy-driven model of type Ia supernova luminosity variations

Author: Wiseman, P., Vincenzi, M., Sullivan, M., Kelsey, L., Popovic, B., Rose, B., Brout, D., Davis, T. M., Frohmaier, C., Galbany, L., Lidman, C., Möller, A., Scolnic, D., Smith, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Varga, T. N., DES Collaboration, Wiseman, P., Vincenzi, M., Sullivan, M., Kelsey, L., Popovic, B., Rose, B., Brout, D., Davis, T. M., Frohmaier, C., Galbany, L., Lidman, C., Möller, A., Scolnic, D., Smith, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Varga, T. N., Des, Collaboration, Science and Technology Facilities Council (UK), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Consejo Superior de Investigaciones Científicas (España), European Research Council, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), and Generalitat de Catalunya
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), supernovae general, dust, extinction, galaxies evolution, cosmology observations, Cosmology: observations, Supernovae: general, Galaxies: evolution, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: P. Wiseman et al., Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U−R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U−R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age., P.W. acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. MS acknowledges support from EU/FP7-ERC grant 615929. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Social Fund (ESF) ‘Investing in your future’ under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement number 759194 - USNAC). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

14. Dark Energy Survey Year 3 results: A 2.7% measurement of baryon acoustic oscillation distance scale at redshift 0.835

Author: Abbott, T.M.C., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Asorey, J., Avila, S., Bernstein, G.M., Bertin, E., Brandao-Souza, A., Brooks, D., Burke, D.L., Calcino, J., Camacho, H., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F.J., Cawthon, R., Chan, K.C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., da Costa, L.N., Pereira, M.E.S., Davis, T.M., De Vicente, J., Desai, S., Diehl, H.T., Doel, P., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A.E., Fang, X., Ferrero, Ismael, Ferté, A., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Glazebrook, K., Gomes, D., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hinton, S.R., Hollowood, D.L., Honscheid, K., Huterer, D., Jain, B., James, D.J., Jeltema, T., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lewis, G.F., Lidman, C., Lima, M., Lin, H., Maia, M.A.G., Malik, U., Martini, P., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J.J., Morgan, R., Muir, J., Myles, J., Möller, A., Palmese, A., Paz-Chinchón, F., Percival, W.J., Pieres, A., Plazas Malagón, A.A., Porredon, A., Prat, J., Reil, K., Rodriguez-Monroy, M., Romer, A.K., Roodman, A., Rosenfeld, R., Ross, A.J., Sanchez, E., Sanchez Cid, D., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., To, C., Troxel, M.A., Tucker, B.E., Tucker, D.L., Tutusaus, I., Uddin, S.A., Varga, T.N., Weller, J., Wilkinson, R.D., UAM. Departamento de Física Teórica, NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia - LIneA, Fermi National Accelerator Laboratory, Stanford University, Universidade Estadual Paulista (UNESP), Medioambientales y Tecnológicas (CIEMAT), Universidad Autonoma de Madrid, University of Pennsylvania, Institut d'Astrophysique de Paris, Universidade Estadual de Campinas (UNICAMP), University College London, SLAC National Accelerator Laboratory, University of Queensland, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, Astrophysical Observatory of Turin, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Wisconsin-Madison, Sun Yat-sen University, The Ohio State University, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, IIT Hyderabad, Santa Cruz Institute for Particle Physics, University of Arizona, University of Oslo, California Institute of Technology, University of Cambridge, Swinburne University of Technology, Universidade de São Paulo (USP), Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, 382 Via Pueblo Mall, Macquarie University, Lowell Observatory, The University of Sydney, The Australian National University, Australian National University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, LPC, University of Chicago, University of Waterloo, Perimeter Institute for Theoretical Physics, University of Sussex, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Duke University Durham, The University of Texas at Austin, Ludwig-Maximilians Universität München, Abbott, T. M. C., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Asorey, J., Avila, S., Bernstein, G. M., Bertin, E., Brandao-Souza, A., Brooks, D., Burke, D. L., Calcino, J., Camacho, H., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chan, K. C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., Da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Glazebrook, K., Gomes, D., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jain, B., James, D. J., Jeltema, T., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Malik, U., Martini, P., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Moller, A., Palmese, A., Paz-Chinchon, F., Percival, W. J., Pieres, A., Plazas Malagon, A. A., Porredon, A., Prat, J., Reil, K., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Sanchez, E., Sanchez Cid, D., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tucker, B. E., Tucker, D. L., Tutusaus, I., Uddin, S. A., Varga, T. N., Weller, J., Wilkinson, R. D., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), DES, National Science Foundation (US), Department of Energy (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Commission, European Research Council, and Generalitat de Catalunya
Subjects: Astrophysic, Halo, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics, Cosmology and Nongalactic Astrophysics, FOS: Physical sciences, Red Shift, Física, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: T. M.C. Abbott et al., We present angular diameter measurements obtained by measuring the position of baryon acoustic oscillations (BAO) in an optimized sample of galaxies from the first three years of Dark Energy Survey data (DES Y3). The sample consists of 7 million galaxies distributed over a footprint of 4100 deg2 with 0.60.75. When combined with DES 3x2pt+SNIa, they lead to improvements in H0 and Ωm constraints by∼20%., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University,the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-20150509, some of which include ERDF funds from the European Union. I.F.A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022
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15. Dark Energy Survey Year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty

Author: Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferté, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sánchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferte, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sanchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Plazas Malagon, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), National Science Foundation (US), European Commission, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, University of Chicago, University of Pennsylvania, Carnegie Mellon University, Northeastern University, University of Arizona, École Polytechnique Fédérale de Lausanne (EPFL), Stanford University, University of Michigan, The Ohio State University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, University of California, California Institute of Technology, University College London, Duke University, University of Cambridge, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, ETH Zürich, Northern Illinois University, University of Zürich, Argonne National Laboratory, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, University of Hawai'i, University of Wisconsin-Madison, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), Instituto de Astrofísica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, University of Manchester, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, Max Planck Institute für Extraterrestrial Physics, Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, Université de Genève, Université de Paris, Laboratoire de Physique de Clermont, Laboratoire de Physique Nucléaire et de Hautes Énergies, The University of Tokyo, Ohio State University, Brookhaven National Laboratory, Ludwig-Maximilians Universität München, NSF's National Optical-Infrared Astronomy Research Laboratory, University of Portsmouth, Institut d'Astrophysique de Paris, University of Sussex, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Max Planck Institute for Extraterrestrial Physics, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A and M University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and UAM. Departamento de Física Teórica
Subjects: luminous red galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, Sky surveys, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Gravitational lenses, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, Weak, baryonic feedback, 010303 astronomy & astrophysics, redshift inference, intrinsic galaxy shapes, Gravitational Lensing, 010308 nuclear & particles physics, Física, COSMOLOGIA, Dark Energy, 13. Climate action, 2-point correlation-functions, photometric data set, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Secco, L.F., et al. (DES Collaboration), This work and its companion paper, Amon et al. [Phys. Rev. D 105, 023514 (2022)PRVDAQ2470-001010.1103/PhysRevD.105.023514], present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter S8σ8ωm/0.3 at the 3% level in ΛCDM: S8=0.759-0.023+0.025 (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the ΛCDM analysis: S8=0.772-0.017+0.018 (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of ΛCDM is found to be in statistical agreement with Planck 2018, although favors a lower S8 than the CMB-inferred value by 2.3σ (a p-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3σ in the plane of S8×ωm caused by uncertainties in the theoretical models., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.
Published: 2022
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16. Dark Energy Survey Year 3 results: Measurement of the baryon acoustic oscillations with three-dimensional clustering

Author: Chan, K. C., Avila, S., Carnero Rosell, A., Ferrero, I., Elvin-Poole, J., Sanchez, E., Camacho, H., Porredon, A., Crocce, M., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Raveri, M., Rodriguez-Monroy, M., Roodman, A., Ross, A. J., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vincenzi, M., Weaverdyck, N., Des, Collaboration, Chan, K. C., Avila, S., Carnero Rosell, A., Ferrero, I., Elvin-Poole, J., Sanchez, E., Camacho, H., Porredon, A., Crocce, M., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Raveri, M., Rodriguez-Monroy, M., Roodman, A., Ross, A. J., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vincenzi, M., Weaverdyck, N., Des, Collaboration, National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Comunidad de Madrid, Department of Energy (US), Ministerio de Educación y Ciencia (España), Science and Technology Facilities Council (UK), Generalitat de Catalunya, and HEP, INSPIRE
Subjects: Astrophysic, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics, Cosmology and Nongalactic Astrophysics, FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: K. C. Chan et al., The three-dimensional correlation function offers an effective way to summarize the correlation of the large-scale structure even for imaging galaxy surveys. We have applied the projected three-dimensional correlation function, ξp to measure the baryonic acoustic oscillations (BAO) scale on the first-three years Dark Energy Survey data. The sample consists of about 7 million galaxies in the redshift range 0.6, K. C.C. acknowledges the support from the National Science Foundation of China under the Grants No. 11873102 and No. 12273121, the science research grants from the China Manned Space Project with No. CMS-CSST-2021-B01, and the Science and Technology Program of Guangzhou, China (Grant No. 202002030360). S.A. is supported by the Spanish Agencia Estatal de Investigacion through the grant “IFT Centro de Excelencia Severo Ochoa by CEX2020-001007-S” and “EU-HORIZON-2020-776247 Enabling Weak Lensing Cosmology (EWC)”, and was also supported by Atraccion de Talento Program No. 2019-T1/TIC-12702 granted by the Comunidad de Madrid in Spain. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at UrbanaChampaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Minist´erio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ´eticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-20150509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (No. FP7/20072013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022
Full Text: View/download PDF

17. Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps

Author: Gatti, M., Jain, B., Chang, C., Raveri, M., Zürcher, D., Secco, L., Whiteway, L., Jeffrey, N., Doux, C., Kacprzak, T., Bacon, D., Fosalba, P., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Campos, A., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Krause, E., Leget, P. F., Lemos, P., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro, A., Pandey, S., Prat, J., Rollins, R. P., Roodman, A., Sanchez, C., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Ferrero, I., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Rodriguez-Monroyv, M., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., DES Collaboration, Gatti, M., Jain, B., Chang, C., Raveri, M., Zürcher, D., Secco, L., Whiteway, L., Jeffrey, N., Doux, C., Kacprzak, T., Bacon, D., Fosalba, P., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Campos, A., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Krause, E., Leget, P. F., Lemos, P., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro, A., Pandey, S., Prat, J., Rollins, R. P., Roodman, A., Sanchez, C., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Ferrero, I., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Rodriguez-Monroyv, M., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Des, Collaboration, UAM. Departamento de Física Teórica, Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Agencia Estatal de Investigación (España), Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Department of Energy (US), National Aeronautics and Space Administration (US), and National Science Foundation (US)
Subjects: Gravitational Lensing, data-compression, inference, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Física, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, parameter-estimation, universe, Dark Energy, Astrophysic, cosmic shear 2-point, model predictions, galaxy, simulations, Weak, peak statistics, constraints, Cosmology and Nongalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: M. Gatti et al., We present a cosmological analysis using the second and third moments of the weak lensing mass (convergence) maps from the first three years of data (Y3) data of the Dark Energy Survey. The survey spans an effective area of 4139 square degrees and uses the images of over 100 million galaxies to reconstruct the convergence field. The second moment of the convergence as a function of smoothing scale contains information similar to standard shear 2-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The data is analyzed in the context of the ΛCDM model, varying five cosmological parameters and 19 nuisance parameters modeling astrophysical and measurement systematics. Our modeling of the observables is completely analytical, and has been tested with simulations in our previous methodology study. We obtain a 1.7% measurement of the amplitude of fluctuations parameter S8≡σ8(Ωm/0.3)0.5=0.784±0.013. The measurements are shown to be internally consistent across redshift bins, angular scales, and between second and third moments. In particular, the measured third moment is consistent with the expectation of gravitational clustering under the ΛCDM model. The addition of the third moment improves the constraints on S8 and Ωm by ∼15% and ∼25% compared to an analysis that only uses second moments. We compare our results with Planck constraints from the cosmic microwave background, finding a 2.2–2.8σ tension in the full parameter space, depending on the combination of moments considered. The third moment, independently, is in 2.8σ tension with Planck, and thus provides a cross-check on the analyses of 2-point correlations., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

18. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Bhargava, S., Birrer, S., Blazek, J., Brandao-Souza, A., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. da Silva, Davis, C., Davis, T. M., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Farahi, A., Fernandez, E., Ferrero, I., Fert��, A., Fosalba, P., Friedrich, O., Frieman, J., Garc��a-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Leget, P. -F., Lemos, P., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., McCullough, J., Melchior, P., Mena-Fern��ndez, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paz-Chinch��n, F., Petravick, D., Pieres, A., Malag��n, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., S��nchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tucker, D. L., Tutusaus, I., Varga, T. N., Walker, A. R., Weaverdyck, N., Wechsler, R., Weller, J., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Bhargava, S., Birrer, S., Blazek, J., Brandao-Souza, A., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., Da Costa, L. N., Da Silva Pereira, M. E., Davis, C., Davis, T. M., De Vicente, J., Derose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Farahi, A., Fernandez, E., Ferrero, I., Ferte, A., Fosalba, P., Friedrich, O., Frieman, J., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Leget, P. -F., Lemos, P., Liddle, A. R., Lidman, C., Lima, M., Lin, H., Maccrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., Mccullough, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paz-Chinchon, F., Petravick, D., Pieres, A., Plazas Malagon, A. A., Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sanchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scarpine, V., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tucker, D. L., Tutusaus, I., Varga, T. N., Walker, A. R., Weaverdyck, N., Wechsler, R., Weller, J., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), Department of Energy (US), Generalitat de Catalunya, National Aeronautics and Space Administration (US), National Science Foundation (US), NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia - LIneA, Argonne National Laboratory, Fermi National Accelerator Laboratory, University of Michigan, Universidade Estadual Paulista (UNESP), Stanford University, Universidad Autonoma de Madrid, University of Portsmouth, University of Hawai'i, University of Wisconsin-Madison, University of Pennsylvania, University of Sussex, 450 Serra Mall, Northeastern University, Observatoire de Sauverny, Universidade Estadual de Campinas (UNICAMP), University of Manchester, University College London, University of Chicago, SLAC National Accelerator Laboratory, Carnegie Mellon University, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Duke University, The Ohio State University, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, Medioambientales y Tecnológicas (CIEMAT), Lawrence Berkeley National Laboratory, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Arizona, California Institute of Technology, Santa Cruz Institute for Particle Physics, University of Texas at Austin, University of Oslo, University of Cambridge, 382 Via Pueblo Mall, Denys Wilkinson Building, University of Geneva, Center for Astrophysics and Harvard and Smithsonian, Université de Paris, Macquarie University, Lowell Observatory, University of Edinburgh, Universidade de Lisboa, Perimeter Institute for Theoretical Physics, The Australian National University, Australian National University, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, The University of Tokyo, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, Ludwig-Maximilians Universität München, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), DES, UAM. Departamento de Física Teórica, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: luminous red galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, parameter constraints, supernova legacy survey, Astrophysics, 01 natural sciences, Astrophysic, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, LENTES GRAVITACIONAIS, Weak, 010303 astronomy & astrophysics, mass correlation-function, Gravitational Lensing, extragalactic objects, 010308 nuclear & particles physics, Física, Dark Energy, ia supernovae, digital sky survey, power-spectrum, photometric data set, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: T. M. C. Abbott et al., We present the first cosmology results from large-scale structure using the full 5000 deg2 of imaging data from the Dark Energy Survey (DES) Data Release 1. We perform an analysis of large-scale structure combining three two-point correlation functions (3×2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions, galaxy–galaxy lensing. To achieve the cosmological precision enabled by these measurements has required updates to nearly every part of the analysis from DES Year 1, including the use of two independent galaxy clustering samples, modeling advances, and several novel improvements in the calibration of gravitational shear and photometric redshift inference. The analysis was performed under strict conditions to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results and tests of the robustness of our results to this decision. We model the data within the flat ΛCDM and wCDM cosmological models, marginalizing over 25 nuisance parameters. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude S8=0.776+0.017−0.017 and matter density Ωm=0.339+0.032−0.031 in ΛCDM, mean with 68% confidence limits; S8=0.775+0.026−0.024, Ωm=0.352+0.035−0.041, and dark energy equation-of-state parameter w=−0.98+0.32−0.20 in wCDM. These constraints correspond to an improvement in signal-to-noise of the DES Year 3 3×2pt data relative to DES Year 1 by a factor of 2.1, about 20% more than expected from the increase in observing area alone. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed p=0.13–0.48. We find better agreement between DES 3×2pt and Planck than in DES Y1, despite the significantly improved precision of both. When combining DES 3×2pt data with available baryon acoustic oscillation, redshift-space distortion, and type Ia supernovae data, we find p=0.34. Combining all of these datasets with Planck CMB lensing yields joint parameter constraints of S8=0.812+0.008−0.008, Ωm=0.306+0.004−0.005, h=0.680+0.004−0.003, and ∑mν, Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478.We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. This work also used resources on Duke Compute Cluster (DCC), the CCAPP condo of the Ruby Cluster at the Ohio Supercomputing Center [232], and computing resources at SLAC National Accelerator Laboratory. We also thank the staff of the Fermilab Computing Sector for their support. Plots in this manuscript were produced partly with MATPLOTLIB [233], and it has been prepared using NASA’s Astrophysics Data System Bibliographic Services.
Published: 2022

19. Dark energy survey year 3 results: High-precision measurement and modeling of galaxy-galaxy lensing

Author: Prat, J., Blazek, J., Sánchez, C., Tutusaus, I., Pandey, S., Elvin-Poole, J., Krause, E., Troxel, M. A., Secco, L. F., Amon, A., Derose, J., Zacharegkas, G., Chang, C., Jain, B., Maccrann, N., Park, Y., Sheldon, E., Giannini, G., Bocquet, S., To, C., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crocce, M., Davis, C., De Vicente, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Fang, X., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Shin, T., Troja, A., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Plazas Malagón, A. A., Sanchez, E., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., Des, Collaboration, A Prat, J., Blazek, J., Sánchez, C., Tutusaus, I., Pandey, S., Elvin- Poole, J., Krause, E., Troxel, M. A., Secco, L. F., Amon, A., Derose, J., Zacharegkas, G., Chang, C., Jain, B., Maccrann, N., Park, Y., Sheldon, E., Giannini, G., Bocquet, S., To, C., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crocce, M., Davis, C., De Vicente, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Fang, X., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Mccullough, J., Muir, J., Myles, J., Navarro- Alsina, A., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Shin, T., Troja, A., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Plazas Malagón, A. A., Sanchez, E., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmological parameter constraints, FOS: Physical sciences, Física, marginalization, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics, Dark Energy, Astrophysic, Cosmology and Nongalactic Astrophysics, redshift distribution, mass, Weak, photometric data set, sdss, cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics, intrinsic alignments
Abstract: DES Collaboration: J. Prat et al., We present and characterize the galaxy-galaxy lensing signal measured using the first three years of data from the Dark Energy Survey (DES Y3) covering 4132 deg2. These galaxy-galaxy measurements are used in the DES Y3 3×2pt cosmological analysis, which combines weak lensing and galaxy clustering information. We use two lens samples: a magnitude-limited sample and the redmagic sample, which span the redshift range ∼0.2–1 with 10.7 and 2.6 M galaxies, respectively. For the source catalog, we use the metacalibration shape sample, consisting of ≃100M galaxies separated into four tomographic bins. Our galaxy-galaxy lensing estimator is the mean tangential shear, for which we obtain a total SNR of ∼148 for maglim (∼120 for redmagic), and ∼67 (∼55) after applying the scale cuts of 6Mpc/h. Thus we reach percent-level statistical precision, which requires that our modeling and systematic-error control be of comparable accuracy. The tangential shear model used in the 3×2pt cosmological analysis includes lens magnification, a five-parameter intrinsic alignment model, marginalization over a point mass to remove information from small scales and a linear galaxy bias model validated with higher-order terms. We explore the impact of these choices on the tangential shear observable and study the significance of effects not included in our model, such as reduced shear, source magnification, and source clustering. We also test the robustness of our measurements to various observational and systematics effects, such as the impact of observing conditions, lens-source clustering, random-point subtraction, scale-dependent metacalibration responses, point spread function residuals, and B modes.
Published: 2022

20. Robust sampling for weak lensing and clustering analyses with the dark energy survey

Author: Lemos, P., Weaverdyck, N., Rollins, R. P., Muir, J., Ferté, A., Liddle, A. R., Campos, A., Huterer, D., Raveri, M., Zuntz, J., Di Valentino, E., Fang, X., Hartley, W. G., Aguena, M., Allam, S., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Dietrich, J. P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., DES Collaboration, Lemos, P., Weaverdyck, N., Rollins, R. P., Muir, J., Ferté, A., Liddle, A. R., Campos, A., Huterer, D., Raveri, M., Zuntz, J., Di Valentino, E., Fang, X., Hartley, W. G., Aguena, M., Allam, S., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Dietrich, J. P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plaza, Porredon, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., and Des, Collaboration
Subjects: methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), statistical [methods], cosmological parameter [cosmology], FOS: Physical sciences, Astronomy and Astrophysics, cosmology: large-scale structure of the Universe, cosmology: cosmological parameters, cosmology: observations, Space and Planetary Science, large-scale structure of the Universe [cosmology], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Recent cosmological analyses rely on the ability to accurately sample from high-dimensional posterior distributions. A variety of algorithms have been applied in the field, but justification of the particular sampler choice and settings is often lacking. Here we investigate three such samplers to motivate and validate the algorithm and settings used for the Dark Energy Survey (DES) analyses of the first 3 years (Y3) of data from combined measurements of weak lensing and galaxy clustering. We employ the full DES Year 1 likelihood alongside a much faster approximate likelihood, which enables us to assess the outcomes from each sampler choice and demonstrate the robustness of our full results. We find that the ellipsoidal nested sampling algorithm $\texttt{MultiNest}$ reports inconsistent estimates of the Bayesian evidence and somewhat narrower parameter credible intervals than the sliced nested sampling implemented in $\texttt{PolyChord}$. We compare the findings from $\texttt{MultiNest}$ and $\texttt{PolyChord}$ with parameter inference from the Metropolis-Hastings algorithm, finding good agreement. We determine that $\texttt{PolyChord}$ provides a good balance of speed and robustness, and recommend different settings for testing purposes and final chains for analyses with DES Y3 data. Our methodology can readily be reproduced to obtain suitable sampler settings for future surveys., 16 pages, 11 figures
Published: 2022

21. Dark Energy Survey Year 3 results: Cosmology with peaks using an emulator approach

Author: Zürcher, D., Fluri, J., Sgier, R., Kacprzak, T., Gatti, M., Doux, C., Whiteway, L., Réfrégier, A., Chang, C., Jeffrey, N., Jain, B., Lemos, P., Bacon, D., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Campos, A., Chen, R., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Leget, P. F., MacCrann, N., McCullough, J., Muir, J., Myles, J., Navarro Alsina, A., Pandey, S., Prat, J., Raveri, M., Rollins, R. P., Roodman, A., Sanchez, C., Secco, L. F., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F. [UNESP], Annis, J., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Cawthon, R., Conselice, C., Costanzi, M., Da Costa, L., Da Silva Pereira, M. E., Davis, T., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J., Doel, P., Eckert, K., Evrard, A., Ferrero, I., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D., Giannantonio, T., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Maia, M., Marshall, J., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagón, A., Reil, K., Rodriguez Monroy, M., Romer, K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Wilkinson, R., National Science Foundation (US), Department of Energy (US), Swiss National Science Foundation, Ministerio de Educación y Ciencia (España), ETH Zurich, National Aeronautics and Space Administration (US), UAM. Departamento de Física Teórica, Zurcher, D., Fluri, J., Sgier, R., Kacprzak, T., Gatti, M., Doux, C., Whiteway, L., Refregier, A., Chang, C., Jeffrey, N., Jain, B., Lemos, P., Bacon, D., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Campos, A., Chen, R., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Leget, P. F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro Alsina, A., Pandey, S., Prat, J., Raveri, M., Rollins, R. P., Roodman, A., Sanchez, C., Secco, L. F., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Cawthon, R., Conselice, C., Costanzi, M., Da Costa, L., Da Silva Pereira, M. E., Davis, T., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J., Doel, P., Eckert, K., Evrard, A., Ferrero, I., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D., Giannantonio, T., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Maia, M., Marshall, J., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Reil, K., Rodriguez Monroy, M., Romer, K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Wilkinson, R., Eth Zuurich, University of Pennsylvania, University College London, University of Chicago, University of Sussex, Université de Paris, University of Portsmouth, Argonne National Laboratory, Stanford University, University of WisconsinMadison, Carnegie Mellon University, Duke University, The Ohio State University, Lawrence Berkeley National Laboratory, Santa Cruz Institute for Particle Physics, California Institute of Technology, Ludwig-Maximilians-Universitat, Denys Wilkinson Building, University of Manchester, University of Michigan, University of Cambridge, Perimeter Institute for Theoretical Physics, 382 Via Pueblo Mall, Slac National Accelerator Laboratory, Universidade Estadual de Campinas (UNICAMP), Bldg 510, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Laboratorio Interinstitucional de E-Astronomia-LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatorio Nacional, Universitat Hamburg, University of Queensland, Medioambientales y Tecnologicas (CIEMAT), Iit Hyderabad, University of Oslo, Universidad Autonoma de Madrid, Harvard and Smithsonian, Macquarie University, Lowell Observatory, The Australian National University, Australian National University, Universidade de São Paulo (USP), Texas A &m University, Peyton Hall, Institucio Catalana de Recerca i Estudis Avancats, 501 Campbell Hall, University of Southampton, Oak Ridge National Laboratory, Max Planck Institute for Extraterrestrial Physics, and Ludwig-Maximilians Universitat Munchen
Subjects: Gravitational Lensing, Cosmology, observations, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: observations, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Dark Energy, Observations [Cosmology], Space and Planetary Science, Weak, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: D. Zürcher et al., We constrain the matter density Ωm and the amplitude of density fluctuations σ8 within the ΛCDM cosmological model with shear peak statistics and angular convergence power spectra using mass maps constructed from the first three years of data of the Dark Energy Survey (DES Y3). We use tomographic shear peak statistics, including cross-peaks: peak counts calculated on maps created by taking a harmonic space product of the convergence of two tomographic redshift bins. Our analysis follows a forward-modelling scheme to create a likelihood of these statistics using N-body simulations, using a Gaussian process emulator. We take into account the uncertainty from the remaining, largely unconstrained ΛCDM parameters (Ωb, ns, and h). We include the following lensing systematics: multiplicative shear bias, photometric redshift uncertainty, and galaxy intrinsic alignment. Stringent scale cuts are applied to avoid biases from unmodelled baryonic physics. We find that the additional non-Gaussian information leads to a tightening of the constraints on the structure growth parameter yielding S8 ≡ σ8 √ Ωm/0.3 = 0.797+0.015−0.013 (68 per cent confidence limits), with a precision of 1.8 per cent, an improvement of 38 per cent compared to the angular power spectra only case. The results obtained with the angular power spectra and peak counts are found to be in agreement with each other and no significant difference in S8 is recorded. We find a mild tension of 1.5σ between our study and the results from Planck 2018, with our analysis yielding a lower S8. Furthermore, we observe that the combination of angular power spectra and tomographic peak counts breaks the degeneracy between galaxy intrinsic alignment AIA and S8, improving cosmological constraints. We run a suite of tests concluding that our results are robust and consistent with the results from other studies using DES Y3 data., The ETH Zurich Cosmology group acknowledges support by grants 200021_192243 and 200021_169130 of the Swiss National Science Foundation. We would also like to thank Uwe Schmitt from ETH Zürich for his support with the GitLab server and CI engine. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physic at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenoessische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Fisica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität Muenchen and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop.ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Based on observations obtained with Planck,11 an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada.
Published: 2021

22. The DECam Local Volume Exploration Survey Data Release 2

Author: Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and Fundação de Amparo à Pesquisa do Estado de São Paulo
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Surveys, Astrophysics - Astrophysics of Galaxies, Catalogs, Local Group, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Catalog, Survey, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Full list of authors: Drlica-Wagner, A.; Ferguson, P. S.; Adamow, M.; Aguena, M.; Allam, S.; Andrade-Oliveira, F.; Bacon, D.; Bechtol, K.; Bell, E. F.; Bertin, E.; Bilaji, P.; Bocquet, S.; Bom, C. R.; Brooks, D.; Burke, D. L.; Carballo-Bello, J. A.; Carlin, J. L.; Carnero Rosell, A.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cerny, W.; Chang, C.; Choi, Y.; Conselice, C.; Costanzi, M.; Crnojevic, D.; da Costa, L. N.; De Vicente, J.; Desai, S.; Esteves, J.; Everett, S.; Ferrero, I; Fitzpatrick, M.; Flaugher, B.; Friedel, D.; Frieman, J.; Garcia-Bellido, J.; Gatti, M.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Hartley, W. G.; Hernandez-Lang, D.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hughes, A. K.; Jacques, A.; James, D. J.; Johnson, M. D.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lidman, C.; Lin, H.; March, M.; Marshall, J. L.; Martinez-Delgado, D.; Martinez-Vazquez, C. E.; Massana, P.; Mau, S.; McNanna, M.; Melchior, P.; Menanteau, F.; Miller, A. E.; Miquel, R.; Mohr, J. J.; Morgan, R.; Mutlu-Pakdil, B.; Munoz, R. R.; Neilsen, E. H.; Nidever, D. L.; Nikutta, R.; Nilo Castellon, J. L.; Noel, N. E. D.; Ogando, R. L. C.; Olsen, K. A. G.; Pace, A. B.; Palmese, A.; Paz-Chinchon, F.; Pereira, M. E. S.; Pieres, A.; Malagon, A. A. Plazas; Prat, J.; Riley, A. H.; Rodriguez-Monroy, M.; Romer, A. K.; Roodman, A.; Sako, M.; Sakowska, J. D.; Sanchez, E.; Sanchez, F. J.; Sand, D. J.; Santana-Silva, L.; Santiago, B.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I; Simon, J. D.; Smith, M.; Soares-Santos, M.; Stringfellow, G. S.; Suchyta, E.; Suson, D. J.; Tan, C. Y.; Tarle, G.; Tavangar, K.; Thomas, D.; To, C.; Tollerud, E. J.; Troxel, M. A.; Tucker, D. L.; Varga, T. N.; Vivas, A. K.; Walker, A. R.; Weller, J.; Wilkinson, R. D.; Wu, J. F.; Yanny, B.; Zaborowski, E.; Zenteno, A.; DELVE Collaboration; DES Collaboration; Astro Data Lab.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ∼160,000 exposures that cover >21,000 deg2 of the high-Galactic-latitude (∣b∣ > 10°) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ∼2.5 billion astronomical sources with a median 5σ point-source depth of g = 24.3, r = 23.9, i = 23.5, and z = 22.8 mag. A region of ∼17,000 deg2 has been imaged in all four filters, providing four-band photometric measurements for ∼618 million astronomical sources. DELVE DR2 covers more than 4 times the area of the previous DELVE data release and contains roughly 5 times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform. © 2022. The Author(s). Published by the American Astronomical Society., The DELVE project is partially supported by Fermilab LDRD project L2019-011, the NASA Fermi Guest Investigator Program Cycle 9 grant 91201, and the National Science Foundation (NSF) under grant AST-2108168. This work is supported by the Fermilab Visiting Scholars Award Program from the Universities Research Association. A.B.P. acknowledges support from NSF grant AST-1813881. J.L.C. acknowledges support from NSF grant AST-1816196. J.D.S. acknowledges support from NSF grant AST-1714873. S.R.M. acknowledges support from NSF grant AST-1909497. D.J.S. acknowledges support from NSF grants AST-1821967 and AST-1813708. D.C. acknowledges support from NSF grant AST-1814208. B.M.P. acknowledges support from the NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2001663. S.M. acknowledges support from the NSF Graduate Research Fellowship under grant DGE-1656518. D.M.D. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Centre of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). C.P.M.B. and M.R.L.C. acknowledge support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement no. 682115). L.S.S. acknowledges the financial support from FAPESP through the grant #2020/03301-5. J.A.C.B. acknowledges support from ANID FONDECYT Regular 1220083. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo á Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2022
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23. Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration

Author: Amon, A., Gruen, D., Troxel, M. A., MacCrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., DeRose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferté, A., Raveri, M., Lemos, P., Campos, A., Prat, J., Sánchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P. -F., Liddle, A. R., McCullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Generalitat de Catalunya, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Amon, A., Gruen, D., Troxel, M. A., Maccrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., Derose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferte, A., Lemos, P., Raveri, M., Campos, A., Prat, J., Sanchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P., Liddle, A. R., Mccullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Tarle, G., Thomas, D., To, C., Weller, J., Stanford University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, Duke University, University of Cambridge, Carnegie Mellon University, The Ohio State University, University of Pennsylvania, University of Chicago, University of Arizona, University of Manchester, Lawrence Berkeley National Laboratory, Universidade Estadual de Campinas (UNICAMP), Laboratório Interinstitucional de E-Astronomia, Observatoire de Sauverny, Argonne National Laboratory, California Institute of Technology, University College London, University of Sussex, University of Michigan, Universidade Estadual Paulista (UNESP), University of Wisconsin-Madison, Instituto de Astrofisica de Canarias, Universidad de la Laguna, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Fermi National Accelerator Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Geneva, University of Edinburgh, Universidade de Lisboa, Perimeter Institute for Theoretical Physics, The University of Tokyo, ETH Zurich, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, University of Portsmouth, Institut d'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics|Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), microwave background anisotropies, systematic-errors, FOS: Physical sciences, parameter constraints, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, internal consistency, Weak, redshift distributions, 010303 astronomy & astrophysics, Gravitational Lensing, 010308 nuclear & particles physics, Física, Dark Energy, intrinsic correlation, matter power spectrum, 2-point correlation-functions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Amon et al., This work, together with its companion paper, Secco, Samuroff et al. [Phys. Rev. D 105, 023515 (2022)], present the Dark Energy Survey Year 3 cosmic-shear measurements and cosmological constraints based on an analysis of over 100 million source galaxies. With the data spanning 4143 deg2 on the sky, divided into four redshift bins, we produce a measurement with a signal-to-noise of 40. We conduct a blind analysis in the context of the Lambda-Cold Dark Matter (ΛCDM) model and find a 3% constraint of the clustering amplitude, S8≡σ8(Ωm/0.3)0.5=0.759+0.025−0.023. A ΛCDM-Optimized analysis, which safely includes smaller scale information, yields a 2% precision measurement of S8=0.772+0.018−0.017 that is consistent with the fiducial case. The two low-redshift measurements are statistically consistent with the Planck Cosmic Microwave Background result, however, both recovered S8 values are lower than the high-redshift prediction by 2.3σ and 2.1σ (p-values of 0.02 and 0.05), respectively. The measurements are shown to be internally consistent across redshift bins, angular scales and correlation functions. The analysis is demonstrated to be robust to calibration systematics, with the S8 posterior consistent when varying the choice of redshift calibration sample, the modeling of redshift uncertainty and methodology. Similarly, we find that the corrections included to account for the blending of galaxies shifts our best-fit S8 by 0.5σ without incurring a substantial increase in uncertainty. We examine the limiting factors for the precision of the cosmological constraints and find observational systematics to be subdominant to the modeling of astrophysics. Specifically, we identify the uncertainties in modeling baryonic effects and intrinsic alignments as the limiting systematics., This research manuscript made use of Astropy [204,205], GetDist [206], ChainConsumer10 [207] and Matplotlib [208], and has been prepared using NASA’s Astrophysics Data System Bibliographic Services. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana- Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, and Office of High Energy Physics.
Published: 2021

24. Dark Energy Survey Year 3 Results: Constraints on cosmological parameters and galaxy bias models from galaxy clustering and galaxy-galaxy lensing using the redMaGiC sample

Author: Pandey, S., Krause, E., DeRose, J., MacCrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., DES Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, European Commission, European Research Council, Pandey, S., Krause, E., Derose, J., Maccrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysic, combination, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Astrophysics of Galaxies, FOS: Physical sciences, marginalization, Astrophysics, Cosmology and Nongalactic Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics - Astrophysics of Galaxies, efficient, Astrophysic, scale dependence, Astrophysics of Galaxies (astro-ph.GA), halo-mass, evolution, impact, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: S. Pandey et al., We constrain cosmological parameters and galaxy-bias parameters using the combination of galaxy clustering and galaxy-galaxy lensing measurements from the Dark Energy Survey (DES) year-3 data. We describe our modeling framework and choice of scales analyzed, validating their robustness to theoretical uncertainties in small-scale clustering by analyzing simulated data. Using a linear galaxy-bias model and redMaGiC galaxy sample, we obtain 10% constraints on the matter density of the Universe. We also implement a nonlinear galaxy-bias model to probe smaller scales that includes parametrization based on hybrid perturbation theory and find that it leads to a 17% gain in cosmological constraining power. We perform robustness tests of our methodology pipeline and demonstrate stability of the constraints to changes in the theory model. Using the redMaGiC galaxy sample as foreground lens galaxies and adopting the best-fitting cosmological parameters from DES year-1 data, we find the galaxy clustering and galaxy-galaxy lensing measurements to exhibit significant signals akin to decorrelation between galaxies and mass on large scales, which is not expected in any current models. This likely systematic measurement error biases our constraints on galaxy bias and the S8 parameter. We find that a scale-, redshift- and sky-area-independent phenomenological decorrelation parameter can effectively capture this inconsistency between the galaxy clustering and galaxy-galaxy lensing. We trace the source of this correlation to a color-dependent photometric issue and minimize its impact on our result by changing the selection criteria of redMaGiC galaxies. Using this new sample, our constraints on the S8 parameter are consistent with previous studies and we find a small shift in the Ωm constraints compared to the fiducial redMaGiC sample. We infer the constraints on the mean host-halo mass of the redMaGiC galaxies in this new sample from the large-scale bias constraints, finding the galaxies occupy halos of mass approximately 1.6×1013M⊙/h., E. K. is supported by the Department of Energy Grant No. DE-SC0020247 and the David and Lucile Packard Foundation. S. P. and B.J. are supported in part by the U.S. Department of Energy Grant No. DE-SC0007901 and NASA ATP Grant No. NNH17ZDA001N. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at The OhioStateUniversity, theMitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ´eticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität MünchenandtheassociatedExcellenceCluster Universe,the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-20160597, and No. MDM-2015-0509, some of which include ERDFfundsfromtheEuropean Union. I.F.A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013) including ERC Grant Agreements No. 240672, No.291329,andNo.306478.Weacknowledgesupportfrom the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office ofScience,OfficeofHighEnergyPhysics.
Published: 2021

25. Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck I: Construction of CMB Lensing Maps and Modeling Choices

Author: Omori, Y., Baxter, E. J., Chang, C., Friedrich, O., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Bleem, L. E., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crawford, T. M., Crocce, M., Davis, C., Derose, J., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Krause, E., Kuropatkin, N., Leget, P. -F, Pablo Lemos, Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sánchez, C., Sanchez, J., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Wu, W. L. K., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Benson, B. A., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carlstrom, J. E., Carretero, J., Chang, C. L., Chown, R., Costanzi, M., Da Costa, L. N., Crites, A. T., Pereira, M. E. S., Haan, T., Vicente, J., Desai, S., Diehl, H. T., Dobbs, M. A., Doel, P., Everett, W., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gaztanaga, E., George, E. M., Giannantonio, T., Halverson, N. W., Hinton, S. R., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., James, D. J., Knox, L., Kuehn, K., Lahav, O., Lee, A. T., Lima, M., Luong-Van, D., March, M., Mcmahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L., Mohr, J. J., Morgan, R., Natoli, T., Padin, S., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Pryke, C., Reichardt, C. L., Romer, A. K., Ruhl, J. E., Sanchez, E., Schaffer, K. K., Schubnell, M., Serrano, S., Shirokoff, E., Smith, M., Staniszewski, Z., Stark, A. A., Suchyta, E., Tarle, G., Thomas, D., To, C., Vieira, J. D., Weller, J., and Williamson, R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Joint analyses of cross-correlations between measurements of galaxy positions, galaxy lensing, and lensing of the cosmic microwave background (CMB) offer powerful constraints on the large-scale structure of the Universe. In a forthcoming analysis, we will present cosmological constraints from the analysis of such cross-correlations measured using Year 3 data from the Dark Energy Survey (DES), and CMB data from the South Pole Telescope (SPT) and Planck. Here we present two key ingredients of this analysis: (1) an improved CMB lensing map in the SPT-SZ survey footprint, and (2) the analysis methodology that will be used to extract cosmological information from the cross-correlation measurements. Relative to previous lensing maps made from the same CMB observations, we have implemented techniques to remove contamination from the thermal Sunyaev Zel'dovich effect, enabling the extraction of cosmological information from smaller angular scales of the cross-correlation measurements than in previous analyses with DES Year 1 data. We describe our model for the cross-correlations between these maps and DES data, and validate our modeling choices to demonstrate the robustness of our analysis. We then forecast the expected cosmological constraints from the galaxy survey-CMB lensing auto and cross-correlations. We find that the galaxy-CMB lensing and galaxy shear-CMB lensing correlations will on their own provide a constraint on $S_8=\sigma_8 \sqrt{\Omega_{\rm m}/0.3}$ at the few percent level, providing a powerful consistency check for the DES-only constraints. We explore scenarios where external priors on shear calibration are removed, finding that the joint analysis of CMB lensing cross-correlations can provide constraints on the shear calibration amplitude at the 5 to 10% level., Comment: 30 pages, 20 figures, To be submitted to PRD
Published: 2022
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26. A measurement of the mean central optical depth of galaxy clusters via the pairwise kinematic Sunyaev-Zel'dovich effect with SPT-3G and DES

Author: Schiappucci, E., Bianchini, F., Aguena, M., Archipley, M., Balkenhol, L., Bleem, L. E., Chaubal, P., Crawford, T. M., Grandis, S., Omori, Y., Reichardt, C. L., Rozo, E., Rykoff, E. S., To, C., Abbott, T. M. C., Ade, P. A. R., Alves, O., Anderson, A. J., Andrade-Oliveira, F., Annis, J., Avva, J. S., Bacon, D., Benabed, K., Bender, A. N., Benson, B. A., Bernstein, G. M., Bertin, E., Bocquet, S., Bouchet, F. R., Brooks, D., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cecil, T. W., Chang, C. L., Chichura, P. M., Chou, T. -L., Costanzi, M., Cukierman, A., da Costa, L. N., Daley, C., de Haan, T., Desai, S., Dibert, K. R., Diehl, H. T., Dobbs, M. A., Doel, P., Doux, C., Dutcher, D., Everett, S., Everett, W., Feng, C., Ferguson, K. R., Ferrero, I., Ferté, A., Flaugher, B., Foster, A., Frieman, J., Galli, S., Gambrel, A. E., García-Bellido, J., Gardner, R. W., Gatti, M., Giannantonio, T., Goeckner-Wald, N., Gruen, D., Gualtieri, R., Guns, S., Gutierrez, G., Halverson, N. W., Hinton, S. R., Hivon, E., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hood, J. C., Huang, N., James, D. J., Knox, L., Korman, M., Kuehn, K., Kuo, C. -L., Lahav, O., Lee, A. T., Lidman, C., Lima, M., Lowitz, A. E., Lu, C., March, M., Mena-Fernández, J., Menanteau, F., Millea, M., Miquel, R., Mohr, J. J., Montgomery, J., Muir, J., Natoli, T., Noble, G. I., Novosad, V., Ogando, R. L. C., Padin, S., Pan, Z., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prabhu, K., Prat, J., Quan, W., Rahlin, A., Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Rouble, M., Ruhl, J. E., Sanchez, E., Scarpine, V., Schubnell, M., Smecher, G., Smith, M., Soares-Santos, M., Sobrin, J. A., Suchyta, E., Suzuki, A., Tarle, G., Thomas, D., Thompson, K. L., Thorne, B., Tucker, C., Umilta, C., Vieira, J. D., Vincenzi, M., Wang, G., Weaverdyck, N., Weller, J., Whitehorn, N., Wu, W. L. K., Yefremenko, V., Young, M. R., and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Física, FOS: Physical sciences, XMM-newton Telescope, Galaxies, Cosmos, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We infer the mean optical depth of a sample of optically selected galaxy clusters from the Dark Energy Survey via the pairwise kinematic Sunyaev-Zel'dovich (KSZ) effect. The pairwise KSZ signal between pairs of clusters drawn from the Dark Energy Survey Year-3 cluster catalog is detected at 4.1 σ in cosmic microwave background temperature maps from two years of observations with the SPT-3G camera on the South Pole Telescope. After cuts, there are 24,580 clusters in the ∼1 ,400 deg2 of the southern sky observed by both experiments. We infer the mean optical depth of the cluster sample with two techniques. The optical depth inferred from the pairwise KSZ signal is τ¯e=(2.97 ±0.73 )×10-3 , while that inferred from the thermal SZ signal is τ¯e=(2.51 ±0.5 5stat±0.1 5syst)×10-3 . The two measures agree at 0.6 σ . We perform a suite of systematic checks to test the robustness of the analysis, The DES participants from Spanish institutions are partially E. SCHIAPPUCCI et al. PHYS. REV. D 107, 042004 (2023) 042004-14 supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-2015- 0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478
Published: 2022
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27. Dark Energy Survey Year 3 Results: Three-Point Shear Correlations and Mass Aperture Moments

Author: Secco, Lucas F., Jarvis, M., Jain, B., Chang, C., Gatti, M., Frieman, J., Adhikari, S., Alarcon, A., Amon, A., Bechtol, K., Becker, M.R., Bernstein, G.M., Blazek, J., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Choi, A., Cordero, J., DeRose, J., Dodelson, S., Doux, C., Drlica-Wagner, A., Everett, S., Giannini, G., Gruen, D., Gruendl, R.A., Harrison, I., Hartley, W.G., Herner, K., Krause, E., MacCrann, N., McCullough, J., Myles, J., Navarro-Alsina, A., Prat, J., Rollins, R.P., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Troxel, M.A., Zeurcher, D., Aguena, M., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D.L., Carretero, J., Castander, F.J., Crocce, M., da Costa, L.N., Pereira, M.E.S., De Vicente, J., Diehl, H.T., Doel, P., Eckert, K., Ferrero, Ismael, Flaugher, B., Friedel, D., García-Bellido, J., Gutierrez, G., Hinton, S.R., Hollowood, D.L., Honscheid, K., Huterer, D., Kuehn, K., Kuropatkin, N., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Mohr, J.J., Morgan, R., Muir, J., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A.A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Serrano, S., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., To, C., Weller, J., National Science Foundation (US), Department of Energy (US), Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Science and Technology Facilities Council (UK), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Generalitat de Catalunya, and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, Quantum Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Física, Molecular, FOS: Physical sciences, prospects, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Dark Energy, Atomic, Nuclear & Particles Physics, weak-lensing surveys, Particle and Plasma Physics, cosmological constraints, cfhtlens, model predictions, Nuclear, Weak, higher-order statistics, cosmic shear, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: L. F. Secco et al., We present high signal-to-noise measurements of three-point shear correlations and the third moment of the mass aperture statistic using the first 3 years of data from the Dark Energy Survey. We additionally obtain the first measurements of the configuration and scale dependence of the four three-point shear correlations which carry cosmological information. With the third-order mass aperture statistic, we present tomographic measurements over angular scales of 4 to 60 arcminutes with a combined statistical significance of 15.0σ. Using the tomographic information and measuring also the second-order mass aperture, we additionally obtain a skewness parameter and its redshift evolution. We find that the amplitudes and scale-dependence of these shear 3pt functions are in qualitative agreement with measurements in a mock galaxy catalog based on N-body simulations, indicating promise for including them in future cosmological analyses. We validate our measurements by showing that B-modes, parity-violating contributions and PSF modeling uncertainties are negligible, and determine that the measured signals are likely to be of astrophysical and gravitational origin., M. J. is supported in part by National Science Foundation Grant No. 1907610. B. J. is supported in part by the U.S. Department of Energy Grant No. DE-SC0007901. C. C. is supported by DOE grant DE-SC0021949. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grants agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). We acknowledge support from the Australian Research Council Centre of Excellence for Allsky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022
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28. Dark Energy Survey Year 3 Results: Constraints on extensions to $Λ$CDM with weak lensing and galaxy clustering

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Alves, O., Amon, A., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S. L., Brooks, D., Burke, D. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, C., Davis, T. M., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huang, H., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P. -F., Lemos, P., Leonard, C. D., Liddle, A. R., Lima, M., Lin, H., MacCrann, N., Marshall, J. L., McCullough, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchón, F., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Scolnic, D., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Yin, B., Zhang, Y., and Zuntz, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences
Abstract: We constrain extensions to the $Λ$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $σ_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $Ω_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(ΔN_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $Σ(k,z) = Σ_0 Ω_Λ(z)/Ω_{Λ,0}$ and $μ(k,z)=μ_0 Ω_Λ(z)/Ω_{Λ,0}$ respectively to $Σ_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(Σ_0,μ_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $Λ$CDM., Updated to match published version. 46 pages, 25 figures, data available at https://dev.des.ncsa.illinois.edu/releases/y3a2/Y3key-extensions
Published: 2022
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29. Dark Energy Survey Year 3 results: Marginalisation over redshift distribution uncertainties using ranking of discrete realisations

Author: Cordero, Juan P., Harrison, Ian, Rollins, Richard P., Bernstein, G. M., Bridle, S. L., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Camacho, H., Campos, A., Choi, A., DeRose, J., Dodelson, S., Eckert, K., Eifler, T. F., Everett, S., Fang, X., Friedrich, O., Gruen, D., Gruendl, R. A., Hartley, W. G., Huff, E. M., Krause, E., Kuropatkin, N., MacCrann, N., McCullough, J., Myles, J., Pandey, S., Raveri, M., Rosenfeld, R., Rykoff, E. S., S��nchez, C., S��nchez, J., Sevilla-Noarbe, I., Sheldon, E., Troxel, M., Wechsler, R., Yanny, B., Yin, B., Zhang, Y., Aguena, M., Allam, S., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L., Pereira, M. E. da Silva, De Vicente, J., Diehl, H. T., Dietrich, J., Doel, P., Elvin-Poole, J., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D., Kuehn, K., Lahav, O., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Palmese, A., Paz-Chinchon, F., Pieres, A., Malag��n, A. Plazas, S��nchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., Varga, T. N., UAM. Departamento de Física Teórica, European Commission, National Aeronautics and Space Administration (US), Agencia Nacional de Investigación y Desarrollo (Chile), Department of Energy (US), National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, Generalitat de Catalunya, The University of Manchester, Denys Wilkinson Building, University of Edinburgh, University of Pennsylvania, Argonne National Laboratory, S/n, Institut d'Estudis Espacials de Catalunya (IEEC), University of Michigan, Universidade Estadual Paulista (UNESP), 382 Via Pueblo Mall, Stanford University, Slac National Accelerator Laboratory, Laboratorio Interinstitucional de E-Astronomia-LIneA, Carnegie Mellon University, The Ohio State University, Santa Cruz Institute for Particle Physics, 501 Campbell Hall, California Institute of Technology, University of Arizona, University of Cambridge, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Université de Geneve, Fermi National Accelerator Laboratory, University of Chicago, Centro de Investigaciones Energeticas Medioambientales y Tecnologicas (CIEMAT), Bldg 510, Duke University, Universidade de São Paulo (USP), Institut d'Astrophysique de Paris, University College London, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, The Barcelona Institute of Science and Technology, University of WisconsinMadison, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Ludwig-Maximilians-Universitat, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universitat Munchen, Center for Astrophysics | Harvard &smithsonian, Macquarie University, Lowell Observatory, Institucio Catalana de Recerca i Estudis Avancats, Perimeter Institute for Theoretical Physics, Observatorio Nacional, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Cordero, J. P., Harrison, I., Rollins, R. P., Bernstein, G. M., Bridle, S. L., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Camacho, H., Campos, A., Choi, A., Derose, J., Dodelson, S., Eckert, K., Eifler, T. F., Everett, S., Fang, X., Friedrich, O., Gruen, D., Gruendl, R. A., Hartley, W. G., Huff, E. M., Krause, E., Kuropatkin, N., Maccrann, N., Mccullough, J., Myles, J., Pandey, S., Raveri, M., Rosenfeld, R., Rykoff, E. S., Sanchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Troxel, M., Wechsler, R., Yanny, B., Yin, B., Zhang, Y., Aguena, M., Allam, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., Da Costa, L., Da Silva Pereira, M. E., De Vicente, J., Diehl, H. T., Dietrich, J., Doel, P., Elvin-Poole, J., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D., Kuehn, K., Lahav, O., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., and Varga, T. N.
Subjects: numerical [Methods], Large-Scale Structure of Universe, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Gravitational Lensing: Weak, distances and redshift [Galaxies], Galaxies: distances and redshifts, Gravitational lensing: weak, Methods: numerical, Física, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxies: Distances and Redshifts, Space and Planetary Science, Methods: Numerical, 0103 physical sciences, distances and redshifts [Galaxies], Large-scale structure of the Universe, weak [Gravitational lensing], 010306 general physics, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: J. P. Cordero et al., Cosmological information from weak lensing surveys is maximized by sorting source galaxies into tomographic redshift subsamples. Any uncertainties on these redshift distributions must be correctly propagated into the cosmological results. We present HYPERRANK, a new method for marginalizing over redshift distribution uncertainties, using discrete samples from the space of all possible redshift distributions, improving over simple parametrized models. In HYPERRANK, the set of proposed redshift distributions is ranked according to a small (between one and four) number of summary values, which are then sampled, along with other nuisance parameters and cosmological parameters in the Monte Carlo chain used for inference. This approach can be regarded as a general method for marginalizing over discrete realizations of data vector variation with nuisance parameters, which can consequently be sampled separately from the main parameters of interest, allowing for increased computational efficiency. We focus on the case of weak lensing cosmic shear analyses and demonstrate our method using simulations made for the Dark Energy Survey (DES). We show that the method can correctly and efficiently marginalize over a wide range of models for the redshift distribution uncertainty. Finally, we compare HYPERRANK to the common mean-shifting method of marginalizing over redshift uncertainty, validating that this simpler model is sufficient for use in the DES Year 3 cosmology results presented in companion papers., This research manuscript made use of ASTROPY (Astropy Collaboration 2013; Astropy Collaboration & Astropy Contributors 2018), ChainConsumer1 (Hinton 2016), and Matplotlib (Hunter 2007), and has been prepared using NASA’s Astrophysics Data System Bibliographic Services. IH, RR, and SB acknowledge support from the European Research Council in the form of a Consolidator Grant with number 681431. IH also acknowledges support from the Beecroft Trust. JPC acknowledges support granted by Agencia Nacional de Investigación y Desarrollo (ANID) DOCTORADO BECAS CHILE/2016 - 72170279. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021
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30. Dark Energy Survey Year 3 Results: Exploiting small-scale information with lensing shear ratios

Author: Sánchez, C., Prat, J., Zacharegkas, G., Pandey, S., Baxter, E., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Krause, E., Lemos, P., Park, Y., Raveri, M., Sanchez, J., Troxel, M. A., Amon, A., Fang, X., Friedrich, O., Gruen, D., Porredon, A., Secco, L. F., Samuroff, S., Alarcon, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Crocce, M., Davis, C., De Vicente, J., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jarvis, M., Jain, B., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Department of Energy (US), Ministerio de Economía y Competitividad (España), European Research Council, Generalitat de Catalunya, European Commission, A Sánchez, C., Prat, J., Zacharegkas, G., Pandey, S., Baxter, E., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Krause, E., Lemos, P., Park, Y., Raveri, M., Sanchez, J., Troxel, M. A., Amon, A., Fang, X., Friedrich, O., Gruen, D., Porredon, A., Secco, L. F., Samuroff, S., Alarcon, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Crocce, M., Davis, C., De Vicente, J., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jarvis, M., Jain, B., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley- Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, mice, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, halo, Física, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics, Dark Energy, Astrophysic, Cosmology and Nongalactic Astrophysics, statistics, galaxies, luminosity, Weak, baryonic feedback, constraints, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], intrinsic alignments, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: C. Sánchez et al., Using the first three years of data from the Dark Energy Survey (DES), we use ratios of small-scale galaxy-galaxy lensing measurements around the same lens sample to constrain source redshift uncertainties, intrinsic alignments and other systematics or nuisance parameters of our model. Instead of using a simple geometric approach for the ratios as has been done in the past, we use the full modeling of the galaxy-galaxy lensing measurements, including the corresponding integration over the power spectrum and the contributions from intrinsic alignments and lens magnification. We perform extensive testing of the small-scale shear-ratio (SR) modeling by studying the impact of different effects such as the inclusion of baryonic physics, nonlinear biasing, halo occupation distribution descriptions and lens magnification, among others, and using realistic N-body simulations of the DES data. We validate the robustness of our constraints in the data by using two independent lens samples with different galaxy properties, and by deriving constraints using the corresponding large-scale ratios for which the modeling is simpler. The results applied to the DES Y3 data demonstrate how the ratios provide significant improvements in constraining power for several nuisance parameters in our model, especially on source redshift calibration and intrinsic alignments. For source redshifts, SR improves the constraints from the prior by up to 38% in some redshift bins. Such improvements, and especially the constraints it provides on intrinsic alignments, translate to tighter cosmological constraints when shear ratios are combined with cosmic shear and other 2pt functions. In particular, for the DES Y3 data, SR improves S8 constraints from cosmic shear by up to 31%, and for the full combination of probes (3×2pt) by up to 10%. The shear ratios presented in this work are used as an additional likelihood for cosmic shear, 2×2pt and the full 3×2pt in the fiducial DES Y3 cosmological analysis., C. S. is supported by Grant No. AST-1615555 from the U.S. National Science Foundation, and Grant No. DESC0007901 from the U.S. Department of Energy (DOE). J. P. is supported by DOE Grant No. DE-SC0021429. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at UrbanaChampaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DESBrazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State UniverFIG. 16. Correlation matrix for the lensing ratios, on the left panel using the REDMAGIC lens sample and on the right panel using the MAGLIM sample. sity, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under Grants No. AST1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV2012-0234, No. SEV-2016-0597, and No. MDM-20150509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grants Agreement No. 240672, No. 291329, and No. 306478.
Published: 2021
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31. Dark Energy Survey Year 3 Results: Galaxy clustering and systematics treatment for lens galaxy samples

Author: Rodriguez-Monroy M., Weaverdyck N., Elvin-Poole J., Crocce M., Carnero Rosell A., Andrade-Oliveira F., Avila S., Bechtol K., Bernstein G. M., Blazek J., Camacho H., Cawthon R., De Vicente J., Derose J., Dodelson S., Everett S., Fang X., Ferrero I., Ferte A., Friedrich O., Gaztanaga E., Giannini G., Gruendl R. A., Hartley W. G., Herner K., Huff E. M., Jarvis M., Krause E., MacCrann N., Mena-Fernandez J., Muir J., Pandey S., Park Y., Porredon A., Prat J., Rosenfeld R., Ross A. J., Rozo E., Rykoff E. S., Sanchez E., Sanchez Cid D., Sevilla-Noarbe I., Tabbutt M., To C., Wagoner E. L., Wechsler R. H., Aguena M., Allam S., Amon A., Annis J., Bacon D., Baxter E., Bertin E., Bhargava S., Brooks D., Burke D. L., Carrasco Kind M., Carretero J., Castander F. J., Choi A., Conselice C., Costanzi M., Da Costa L. N., Pereira M. E. S., Desai S., Diehl H. T., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Giannantonio T., Gruen D., Gschwend J., Gutierrez G., Hinton S. R., Hollowood D. L., Honscheid K., Huterer D., Jain B., James D. J., Kuehn K., Kuropatkin N., Lima M., Maia M. A. G., March M., Marshall J. L., Melchior P., Menanteau F., Miller C. J., Miquel R., Mohr J. J., Morgan R., Palmese A., Paz-Chinchon F., Pieres A., Plazas Malagon A. A., Roodman A., Scarpine V., Serrano S., Smith M., Soares-Santos M., Suchyta E., Tarle G., Thomas D., Varga T. N., UAM. Departamento de Física Teórica, National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Educación y Ciencia (España), National Aeronautics and Space Administration (US), Generalitat de Catalunya, Medioambientales y Tecnologicas (CIEMAT), University of Michigan, The Ohio State University, Institut d'Estudis Espacials de Catalunya (IEEC), S/n, Instituto de Astrofisica de Canarias, Laboratorio Interinstitucional de E-Astronomia-LIneA, Dpto. Astrofísica, Universidade Estadual Paulista (UNESP), Universidad Autonoma de Madrid, University of WisconsinMadison, University of Pennsylvania, Northeastern University, Observatoire de Sauverny, Lawrence Berkeley National Laboratory, Carnegie Mellon University, Santa Cruz Institute for Particle Physics, University of Arizona, University of Oslo, California Institute of Technology, University of Cambridge, The Barcelona Institute of Science and Technology, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, University of Geneva, Fermi National Accelerator Laboratory, Stanford University, The University of Tokyo, University of Chicago, Slac National Accelerator Laboratory, 382 Via Pueblo Mall, University of Portsmouth, University of Hawai'i, Institut d'Astrophysique de Paris, University of Sussex, University College London, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatorio Nacional, Iit Hyderabad, University of Queensland, Center for Astrophysics | Harvard &smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A &m University, Peyton Hall, Institucio Catalana de Recerca i Estudis Avancats, Ludwig-Maximilians-Universitat, Max Planck Institute for Extraterrestrial Physics, University of Southampton, Oak Ridge National Laboratory, Ludwig-Maximilians Universitat Munchen, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Rodriguez-Monroy, M., Weaverdyck, N., Elvin-Poole, J., Crocce, M., Carnero Rosell, A., Andrade-Oliveira, F., Avila, S., Bechtol, K., Bernstein, G. M., Blazek, J., Camacho, H., Cawthon, R., De Vicente, J., Derose, J., Dodelson, S., Everett, S., Fang, X., Ferrero, I., Ferte, A., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Hartley, W. G., Herner, K., Huff, E. M., Jarvis, M., Krause, E., Maccrann, N., Mena-Fernandez, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Prat, J., Rosenfeld, R., Ross, A. J., Rozo, E., Rykoff, E. S., Sanchez, E., Sanchez Cid, D., Sevilla-Noarbe, I., Tabbutt, M., To, C., Wagoner, E. L., Wechsler, R. H., Aguena, M., Allam, S., Amon, A., Annis, J., Bacon, D., Baxter, E., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Giannantonio, T., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jain, B., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A. A., Roodman, A., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., and Varga, T. N.
Subjects: Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, Observations [Cosmology], Cosmological parameters, Cosmology: observations, Dark energy, Large-scale structure of the Universe, mitigation, 0103 physical sciences, emission, scale structure catalogs, cosmological parameters, dark energy, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, redshift, uncertainties, Dark Energy, Space and Planetary Science, cosmology: observations, Cosmological Parameters, large-scale structure of the universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], constraints, Large-Scale Structure of the Universe, cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: M. Rodríguez-Monroy, N. Weaverdyck, J. Elvin-Poole et al., In this work, we present the galaxy clustering measurements of the two DES lens galaxy samples: a magnitude-limited sample optimized for the measurement of cosmological parameters, MAGLIM, and a sample of luminous red galaxies selected with the REDMAGIC algorithm. MAGLIM/REDMAGIC sample contains over 10 million/2.5 million galaxies and is divided into six/five photometric redshift bins spanning the range z ∈ [0.20, 1.05]/z ∈ [0.15, 0.90]. Both samples cover 4143 deg2 over which we perform our analysis blind, measuring the angular correlation function with an S/N ∼ 63 for both samples. In a companion paper, these measurements of galaxy clustering are combined with the correlation functions of cosmic shear and galaxy–galaxy lensing of each sample to place cosmological constraints with a 3 × 2pt analysis. We conduct a thorough study of the mitigation of systematic effects caused by the spatially varying survey properties and we correct the measurements to remove artificial clustering signals. We employ several decontamination methods with different configurations to ensure the robustness of our corrections and to determine the systematic uncertainty that needs to be considered for the final cosmology analyses. We validate our fiducial methodology using lognormal mocks, showing that our decontamination procedure induces biases no greater than 0.5σ in the (Ωm, b) plane, where b is the galaxy bias., Funding for the Dark Energy Survey Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This paper is based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021
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32. Validation of selection function, sample contamination and mass calibration in galaxy cluster samples

Author: Grandis, S., Klein, M., Mohr, J. J., Bocquet, S., Paulus, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Benson, B. A., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Capasso, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sheldon, E., Smith, M., Stark, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Grandis, S., Klein, M., Mohr, J. J., Bocquet, S., Paulus, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Benson, B. A., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Capasso, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sheldon, E., Smith, M., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R., National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, and European Research Council
Subjects: Software_OPERATINGSYSTEMS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputingMethodologies_SIMULATIONANDMODELING, Calibration (statistics), statistical [methods], RAIOS X, FOS: Physical sciences, Sample (statistics), Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, methods: statistical, galaxies: clusters: general, large-scale structure of Universe, X-rays: galaxies: clusters, Astrophysics - Cosmology and Nongalactic Astrophysics, Hardware_INTEGRATEDCIRCUITS, clusters: general [galaxies], Limit (mathematics), Statistical physics, 010303 astronomy & astrophysics, Selection (genetic algorithm), Galaxy cluster, STFC, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Astronomy and Astrophysics, Function (mathematics), ComputerSystemsOrganization_PROCESSORARCHITECTURES, galaxies: cluster [X-rays], South Pole Telescope, Space and Planetary Science, Outlier, galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al., We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux–mass and richness–mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies., The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union 7th Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2020
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33. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary-Black-hole Merger GW170814

Author: Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D. E, Lin, H, Pereira, M. E. S, Garcia, A, Herner, K, Kessler, R, Peiris, V, H, Sako, M, Allam, S, Brout, D, Carnero Rosell, A, Chen, H. Y, Conselice, C, Derose, J, Devicente, J, Diehl, H. T, Gill, M. S. S, Gschwend, J, Sevilla-Noarbe, I and Tucker, D. L., Wechsler, R, Berger, E, Cowperthwaite, P. S, Metzger, B. D, Williams, P. K. G, Abbott, T. M. C, Abdalla, F. B, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D. L, Kind, Carrasco and Carretero, M., J, Castander, F. J, Crocce, M, Cunha, C. E, D'Andrea, C. B, da Costa, L. N, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T. F, Evrard, A. E, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D. W, Gruen, D, Gruendl, R. A, Gutierrez, G, Hollowood, D. L, Hoyle, B, James, D. J, Jeltema, T, Kuehn, K, Kuropatkin, N, T. S, Li, Lima, M, Maia, M. A. G, Marshall, J. L, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R. L. C, Plazas, A. A, Romer, A. K, Roodman, A, Sanchez, E, Scarpine, V and Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R. C, Sobreira, F, Suchyta, E, Swanson, M. E. C, Tarle, G, Thomas, R. C, Walker, A. R, Wester, W, Zuntz, J, Abbott, B. P, Abbott, R, Abbott, T. D, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M. A, Altin, P. A, Amato, A, Ananyeva, A, Anderson, S. B, Anderson, W. G, Angelova, S, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arene, M, Ascenzi, S, Ashton, G, Aston, S. M, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V and Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M. K. M, Bae, S, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Banagiri, S, Barayoga, J. C, Barclay, S. E, Barish, B. C, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I and Bassiri, Basti, A, Bawaj, M, Bayley, J. C, Bazzan, M, Becsy, B, Bejger, M, Bell, A. S, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J. J, Berry, C. P. L, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I. A, Bilgili, S. A, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J. K, Blair, C. D, Blair, D. G, Blair, R. M, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B. A, Booth, C. D, Bork, R, Boschi, V and Bose, Bossie, K, Bossilkov, V and Bosveld, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P. R, Bramley, A, Branchesi, M, Brau, J. E, Briant, T, Briggs, J. H, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A. F, Brown, D. D, Brunett, S, Buikema, A, Bulik, T, Bulten, H. J, Buonanno, A, Buskulic, D, Buy, C, Byer, R. L, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, Calderon and Callister, J., T. A., Calloni, E, Camp, J. B, Campbell, W. A, Cannon, K. C, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M. F, Carullo, G, Diaz, Casanueva and Casentini, J., C, Caudill, S, Cavaglia, M, Cavalieri, R, Cella, G, Cerda-Duran, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S. J, Chan, M, Chao, S, Charlton, P, Chase, E. A, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B. D, Chen, X, Chen, Y, Cheng, H-P and Cheong, C. K., Chia, H. Y, Chincarini, A, Chiummo, A, Cho, G, Cho, H. S, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K. W, Chung, S, Ciani, G, Ciobanu, A. A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J. A, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Colgan, R, Colleoni, M, Collette, C. G, Collins, C, Cominsky, L. R, Constancio Jr, M, Conti, L, Cooper, S. J, Corban, P, Corbitt, T. R, Cordero-Carrion, I and Corley, K. R., Cornish, N, Corsi, A, Cortese, S, Costa, C. A, Cotesta, R, Coughlin, M. W, Coughlin, S. B, Coulon, J-P and Countryman, S. T., Couvares, P, Covas, P. B, Cowan, E. E, Coward, D. M, Cowart, M. J, Coyne, D. C, Coyne, R, Creighton, J. D. E, Creighton, T. D, Cripe, J, Croquette, M, Crowder, S. G, Cullen, T. J, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, D'Antonio, S, Danilishin, S. L, Danzmann, K, Dasgupta, A, Costa, Da Silva and Datrier, C. F., L. E. H., Dattilo, V and Dave, I and Davis, D, Daw, E. J, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, L. M, Demos, N, Dent, T, De Pietri, R, Derby, J, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, M. C, Dietrich, T, Di Fiore, L, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Palma, Di, I and Di Renzo, F, Dmitriev, A, Donovan, F, Dooley, K. L, Doravari, S, Dorrington, I and Downes, T. P., Drago, M, Driggers, J. C, Du, Z, Dupej, P, Dwyer, S. E, Easter, P. J, Edo, T. B, Edwards, M. C, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S. S, Eisenmann, M, Eisenstein, R. A, Estelles, H, Estevez, D, Etienne, Z. B, Etzel, T, Evans, M, Evans, T. M, Fafone, V and Fair, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon-Jones, E. J, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M. M, Feng, F, Fernandez-Galiana, A, Ferrante, I and Ferreira, E. C., Ferreira, T. A, Ferrini, F, Fidecaro, F, Fiori, I and Fiorucci, Fisher, R. P, Fishner, J. M, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Fournier, J-D and Font, J. A., Forsyth, P. W. F, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H. A, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Ganija, M. R, Gaonkar, S. 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C, Heitmann, H, Hemming, G, Hendry, M, Heng, I. S, Hennig, J, Heptonstall, A. W, Vivanco, Francisco Hernandez and Heurs, M, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A. M, Holland, N. A, Holt, K, Hopkins, P, Horst, C, Hough, J, Howell, E. J, Hoy, C. G, Hreibi, A, Huerta, E. A, Hughey, B, Hulko, M, Husa, S, Huttner, S. H, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isac, J-M and Isa, H. N., Isi, M, Iyer, B. R, Izumi, K, Jacqmin, T, Jadhav, S. J, Jani, K, Janthalur, N. N, Jaranowski, P, Jenkins, A. C, Jiang, J, Johnson, D. S, Jones, A. W, Jones, I, Jones, R, Jonker, R. J. G, Ju, L, Junker, J, Kalaghatgi, Kalogera, V and Kamai, B, Kandhasamy, S, Kang, G, Kanner, J. B, Kapadia, S. J, Karki, S, Karvinen, K. S, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kefelian, F, Keitel, D, Kennedy, R, Key, J. S, Khalili, F. Y, Khan, H, Khan, I and Khan, Khan, Z, Khazanov, E. A, Khursheed, M, Kijbunchoo, N, Kim, Chunglee and Kim, J. C., Kim, K, Y-M and Kim, W, Kim, W. S, Kimball, C, King, E. J, King, P. J, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J. S, Kleybolte, L, Klika, J. H, Klimenko, S, Knowles, T. D, Koch, P, Koehlenbeck, S. M, Koekoek, G, Koley, S, Kondrashov, V and Kontos, Koper, N, Korobko, M, Korth, W. Z, Kowalska, I and Kozak, D. B., Kringel, V and Krishnendu, Krolak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B. D, Lai, K. H, Lam, T. L, Landry, M, Lane, B. B, Lang, R. N, Lange, J, Lantz, B, Lanza, R. K, Lasky, P. D, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y. K, Lee, C. H, Lee, H. K, Lee, H. M, Lee, H. W, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, K. J. L, Li, T. G. F, Li, Li, X, Lin, F, Linde, F, Linker, S. D, Littenberg, T. B, Liu, J, Liu, X, R. K. L, Lo, Lockerbie, N. A, London, L. 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A, Mereni, L, Merilh, E. L, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Metzdorff, R, Meyers, P. M, Miao, H, Michel, C, Middleton, H, Mikhailov, E. E, Milano, L, Miller, A. L, Miller, A, Millhouse, M, Mills, J. C, Milovich-Goff, M. C, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V. P, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, S. R. P, Montani, M, Moore, C. J, Moraru, D, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C. M, Mukherjee, Arunava and Mukherjee, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E. A, Muratore, M, Murray, P. G, Nardecchia, I and Naticchioni, L, Nayak, R. K, Neilson, J, Nelemans, G, Nelson, T. J. N, Nery, M, Neunzert, A, K. Y, Ng, Ng, S, Nguyen, P, Nichols, D, Nissanke, S, Nocera, F, North, C, Nuttall, L. K, Obergaulinger, M, Oberling, J, O'Brien, B. D, O'Dea, G. D, Ogin, G. H, J. J, Oh, S. H, Oh, Ohme, F, Ohta, H, Okada, M. 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J., Quintero, E. A, Quitzow-James, R, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K. E, Ramos-Buades, A, Rana, Javed and Rao, Rapagnani, P, Raymond, V and Razzano, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D. H, Ren, W, Ricci, F, Richardson, C. J, Richardson, J. W, Ricker, P. M, Riles, K, Rizzo, M, Robertson, N. A, Robie, R, Rocchi, A, Rolland, L, Rollins, J. G, Roma, V. J, Romanelli, M, Romano, R, Romel, C. L, Romie, J. H, Rose, K, Rosinska, D, Rosofsky, S. G, Ross, M. P, Rowan, S, Ruediger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E. J, Sanchez, L. E, Sanchis-Gual, N, Sandberg, V and Sanders, J. R., Santiago, K. A, Sarin, N, Sassolas, B, Saulson, P. R, Sauter, O, Savage, R. L, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R. M. S, Schoenbeck, A, Schreiber, E, Schulte, B. W, Schutz, B. F, Schwalbe, S. G, Scott, J, Scott, S. M, Seidel, E, Sellers, D, Sengupta, A. S, Sennett, N, Sentenac, D, Sequino, V and Sergeev, Shaddock, D. A, Shaffer, T, Shahriar, M. S, Shaner, M. B, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D. H, Shoemaker, D. M, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, A. D, Singer, L. P, Singh, N, Singhal, A, Sintes, A. M, Sitmukhambetov, S, Skliris, V and Slagmolen, B. J. J., Slaven-Blair, T. J, Smith, J. R, Smith, R. J. E, Somala, S, Son, E. J, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A. P, Srivastava, A. K, Srivastava, V and Staats, Stachie, C, Standke, M, Steer, D. A, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S. P, Stocks, D, Stone, R, Stops, D. J, Strain, K. A, Stratta, G, Strigin, S. E, Strunk, A, Sturani, R, Stuver, A. L, Sudhir, V and Summerscales, T. Z., Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P. J, Swinkels, B. L, Szczepanczyk, M. J, Tacca, M, Tait, S. C, Talbot, C, Talukder, D, Tanner, D. B, Tapai, M, Taracchini, A, Tasson, J. D, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S. R, Thorne, K. A, Thrane, E, Tiwari, Shubhanshu and Tiwari, Srishti and Tiwari, V and Toland, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, Toyra, D, Travasso, F, Traylor, G, Tringali, M. C, Trovato, A, Trozzo, L, Trudeau, R, Tsang, K. W, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C. S, Urban, A. L, Usman, S. A, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, J. F. J, van den Broeck, C, Vander-Hyde, D. C, Van, Heijningen, van der Schaaf, L, van Veggel, A. A, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P. J, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, A. D, Vine, D. J, Vinet, J-Y and Vitale, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S. P, Wade, A. R, Wade, L. E, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J. Z, Wang, W. H, Wang, Y. F, Ward, R. L, Warden, Z. A, Warner, J, Was, M, Watchi, J, Wei, L-W and Weaver, Weinert, M, Weinstein, A. J, Weiss, R, Wellmann, F, Wen, L, Wessel, E. K, Wessels, P, Westhouse, J. W, Wette, K, Whelan, J. T, Whiting, B. F, Whittle, C, Wilken, D. M, Williams, D, Williamson, A. R, Willis, J. L, Willke, B, Wimmer, M. H, Winkler, W, Wipf, C. C, Wittel, H, Woan, G, Woehler, J, Wofford, J. K, Worden, J, Wright, J. L, D. S, Wu, Wysocki, D. M, Xiao, L, Yamamoto, H, Yancey, C. C, Yang, L, Yap, M. J, Yazback, M, Yeeles, D. W, Hang and Yu, Haocun and Yuen, S. H. R., Yvert, M, Zadrozny, A. K, Zendri, J-P and Zanolin, Zelenova, T, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhou, M, Zhou, Z, Zhu, X. J, Zimmerman, A, Zucker, M. E, Zweizig, J, DES Collaboration and LIGO Sci Collaboration and Virgo Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Collège de France (CdF)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon, ESPCI ParisTech, DES, LIGO Scientific, Virgo, Van Swinderen Institute for Particle Physics and G, Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D, Lin, H, Pereira, M, Garcia, A, Herner, K, Kessler, R, Peiris, H, Sako, M, Allam, S, Brout, D, Rosell, A, Chen, H, Conselice, C, Derose, J, Devicente, J, Diehl, H, Gill, M, Gschwend, J, Sevilla-Noarbe, I, Tucker, D, Wechsler, R, Berger, E, Cowperthwaite, P, Metzger, B, Williams, P, Abbott, T, Abdalla, F, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D, Kind, M, Carretero, J, Castander, F, Crocce, M, Cunha, C, D’Andrea, C, Costa, L, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T, Evrard, A, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Hollowood, D, Hoyle, B, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Li, T, Lima, M, Maia, M, Marshall, J, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R, Plazas, A, Romer, A, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R, Sobreira, F, Suchyta, E, Swanson, M, Tarle, G, Thomas, R, Walker, A, Wester, W, Zuntz, J, Abbott, B, Abbott, R, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R, Adya, V, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M, Altin, P, Amato, A, Ananyeva, A, Anderson, S, Anderson, W, Angelova, S, Appert, S, Arai, K, Araya, M, Areeda, J, Arène, M, Ascenzi, S, Ashton, G, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M, Bae, S, Baker, P, Baldaccini, F, Ballardin, G, Ballmer, S, Banagiri, S, Barayoga, J, Barclay, S, Barish, B, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Bécsy, B, Bejger, M, Bell, A, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I, Bilgili, S, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Booth, C, Bork, R, Boschi, V, Bose, S, Bossie, K, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branchesi, M, Brau, J, Briant, T, Briggs, J, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brown, D, Brunett, S, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buskulic, D, Buy, C, Byer, R, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callister, T, Calloni, E, Camp, J, Campbell, W, Cannon, K, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M, Carullo, G, Diaz, J, Casentini, C, Caudill, S, Cavaglià, M, Cavalieri, R, Cella, G, Cerdá-Durán, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S, Chan, M, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B, Chen, X, Chen, Y, Cheng, H, Cheong, C, Chia, H, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K, Chung, S, Ciani, G, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Cohadon, P, Colgan, R, Colleoni, M, Collette, C, Collins, C, Cominsky, L, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrión, I, Corley, K, Cornish, N, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Couvares, P, Covas, P, Cowan, E, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Cripe, J, Croquette, M, Crowder, S, Cullen, T, Cumming, A, Cunningham, L, Cuoco, E, Canton, T, Dálya, G, Danilishin, S, D’Antonio, S, Danzmann, K, Dasgupta, A, Datrier, L, Dattilo, V, Dave, I, Davis, D, Daw, E, Debra, D, Deenadayalan, M, Degallaix, J, Laurentis, M, Deléglise, S, Pozzo, W, Demarchi, L, Demos, N, Dent, T, Pietri, R, Derby, J, Rosa, R, Rossi, C, Desalvo, R, Varona, O, Dhurandhar, S, Díaz, M, Dietrich, T, Fiore, L, Giovanni, M, Girolamo, T, Lieto, A, Ding, B, Pace, S, Palma, I, Renzo, F, Dmitriev, A, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Downes, T, Drago, M, Driggers, J, Du, Z, Dupej, P, Dwyer, S, Easter, P, Edo, T, Edwards, M, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, E, Ferreira, T, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fisher, R, Fishner, J, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Font, J, Forsyth, P, Fournier, J, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gammaitoni, L, Ganija, M, Gaonkar, S, García-Quirós, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Germain, V, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, J, Giardina, K, Giazotto, A, Gill, K, Giordano, G, Glover, L, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, González, G, Castro, J, Gopakumar, A, Gorodetsky, M, Gossan, S, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, E, Groot, P, Grote, H, Grunewald, S, Guidi, G, Gulati, H, Guo, Y, Gupta, A, Gupta, M, Gustafson, E, Gustafson, R, Haegel, L, Halim, O, Hall, B, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanke, M, Hanks, J, Hanna, C, Hannuksela, O, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heitmann, H, Hemming, G, Hendry, M, Heng, I, Hennig, J, Heptonstall, A, Vivanco, F, Heurs, M, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A, Holland, N, Holt, K, Hopkins, P, Horst, C, Hough, J, Howell, E, Hoy, C, Hreibi, A, Huerta, E, Hughey, B, Hulko, M, Husa, S, Huttner, S, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H, Isac, J, Isi, M, Iyer, B, Izumi, K, Jacqmin, T, Jadhav, S, Jani, K, Janthalur, N, Jaranowski, P, Jenkins, A, Jiang, J, Johnson, D, Jones, A, Jones, D, Jones, R, Jonker, R, Ju, L, Junker, J, Kalaghatgi, C, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, J, Kapadia, S, Karki, S, Karvinen, K, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kéfélian, F, Keitel, D, Kennedy, R, Key, J, Khalili, F, Khan, H, Khan, I, Khan, S, Khan, Z, Khazanov, E, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, E, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, J, Klimenko, S, Knowles, T, Koch, P, Koehlenbeck, S, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, W, Kowalska, I, Kozak, D, Kringel, V, Krishnendu, N, Królak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B, Lai, K, Lam, T, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Lanza, R, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, C, Lee, H, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, Li, K, Li, X, Lin, F, Linde, F, Linker, S, Littenberg, T, Liu, J, Liu, X, Lo, R, Lockerbie, N, London, L, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Lower, M, Lück, H, Lumaca, D, Lundgren, A, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D, Macquet, A, Hernandez, I, Magaña-Sandoval, F, Zertuche, L, Magee, R, Majorana, E, Maksimovic, I, Malik, 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N., Lange, J., Lantz, B., Lanza, R. K., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A., Letendre, N., Levin, Y., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Macinnis, M., Macleod, D. M., Macquet, A., Hernandez, I. Magaña, Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O’Brien, B. D., O’Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R. G., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Shao, L., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Siellez, K., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tápai, M., Taracchini, A., Tasson, J. D., Taylor, R., Thies, F., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Tringali, M. C., Trovato, A., Trozzo, L., Trudeau, R., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Broeck, C. Van Den, Vander-Hyde, D. C., van Heijningen, J. V., van der Schaaf, L., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Weßels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Yvert, M., Zadrożny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A., Zucker, M. E., Zweizig, J., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution))
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, cosmic background radiation, 01 natural sciences, black hole, LIGO, dark energy, 010303 astronomy & astrophysics, gravitational wave, QC, Photometric redshift, QB, Physics, Settore FIS/01, Hubble constant, CATALOG, observations [cosmology], gravitational waves, Physical Sciences, symbols, astro-ph.CO, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, AST-1138766, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, gravitational radiation: direct detection, electromagnetic field: production, symbols.namesake, SDG 17 - Partnerships for the Goals, Binary black hole, statistical analysis, surveys, 0103 physical sciences, supernova, AST-1536171, Luminosity distance, STFC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ONDAS GRAVITACIONAIS, Science & Technology, catalogs, cosmology: observations, gravitational radiation, RCUK, Astronomy and Astrophysics, redshift, Galaxy, Redshift, gravitational radiation detector, VIRGO, Physics and Astronomy, black hole: binary, RESOLUTION, Space and Planetary Science, gravitational radiation: emission, Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract: We present a multi-messenger measurement of the Hubble constant H_0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the LIGO/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black-hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black-hole merger. Our analysis results in $H_0 = 75.2^{+39.5}_{-32.4}~{\rm km~s^{-1}~Mpc^{-1}}$, which is consistent with both SN Ia and CMB measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20,140] ${\rm km~s^{-1}~Mpc^{-1}}$, and it depends on the assumed prior range. If we take a broader prior of [10,220] ${\rm km~s^{-1}~Mpc^{-1}}$, we find $H_0 = 78^{+ 96}_{-24}~{\rm km~s^{-1}~Mpc^{-1}}$ ($57\%$ of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on $H_0$., Comment: 18 pages, 2 Figures, submitted to ApJL
Published: 2019
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34. Noise from undetected sources in Dark Energy Survey images

Author: Eckert, K., Bernstein, G. M., Amara, A., Amon, A., Choi, A., Everett, S., Gruen, D., Gruendl, R. A., Huff, E. M., Kuropatkin, N., Roodman, A., Sheldon, E., Yanny, B., Zhang, Y., Abbott, T. M. C., Aguena, M., Avila, S., Bechtol, K., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kron, R., Kuehn, K., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Zuntz, J., Collaboration, the DES, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, Eckert, K., Bernstein, G. M., Amara, A., Amon, A., Choi, A., Everett, S., Gruen, D., Gruendl, R. A., Huff, E. M., Kuropatkin, N., Roodman, A., Sheldon, E., Yanny, B., Zhang, Y., Abbott, T. M. C., Aguena, M., Avila, S., Bechtol, K., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kron, R., Kuehn, K., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Zuntz, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Diffuse radiation, weak, techniques: image processing, diffuse radiation [gravitational lensing], media_common.quotation_subject, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Poisson distribution, 7. Clean energy, 01 natural sciences, symbols.namesake, weak [gravitational lensing], 0103 physical sciences, Image noise, gravitational lensing: weak, techniques: image processing, diffuse radiation, education, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Weak gravitational lensing, STFC, media_common, Physics, education.field_of_study, image processing [techniques], 010308 nuclear & particles physics, Gravitational lensing: Weak, Shot noise, RCUK, Astronomy and Astrophysics, Techniques: Image processing, Galaxy, diffuse radiation, 13. Climate action, Space and Planetary Science, Sky, symbols, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: For ground-based optical imaging with current CCD technology, the Poisson fluctuations in source and sky background photon arrivals dominate the noise budget and are readily estimated. Another component of noise, however, is the signal from the undetected population of stars and galaxies. Using injection of artifical galaxies into images, we demonstrate that the measured variance of galaxy moments (used for weak gravitational lensing measurements) in Dark Energy Survey (DES) images is significantly in excess of the Poisson predictions, by up to 30 per cent, and that the background sky levels are overestimated by current software. By cross-correlating distinct images of 'empty' sky regions, we establish that there is a significant image noise contribution from undetected static sources (US), which, on average, are mildly resolved at DES resolution. Treating these US as a stationary noise source, we compute a correction to the moment covariance matrix expected from Poisson noise. The corrected covariance matrix matches the moment variances measured on the injected DES images to within 5 per cent. Thus, we have an empirical method to statistically account for US in weak lensing measurements, rather than requiring extremely deep sky simulations. We also find that local sky determinations can remove most of the bias in flux measurements, at a small penalty in additional, but quantifiable, noise., KDE and GMB acknowledge support from NASA through a Research Support Agreement with grant 12-EUCLID11-0004, and grants AST-1615555 from the US National Science Foundation, and DE-SC0007901 from the US Department of Energy. Funding for the DES Projects has been provided by the US Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2020
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35. The DES Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5,000 Sq. Deg. Footprint

Author: O'Donnell, J. H., Wilkinson, R. D., Diehl, H. T., Aros-Bunster, C., Bechtol, K., Birrer, S., Buckley-Geer, E. J., Rosell, A. Carnero, Kind, M. Carrasco, da Costa, L. N., Lozano, S. J. Gonzalez, Gruendl, R. A., Hilton, M., Lin, H., Lindgren, K. A., Martin, J., Pieres, A., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Sif��n, C., Tucker, D. L., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., De Vicente, J., Desai, S., Dietrich, J. P., Eckert, K., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gill, M. S. S., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Nord, B., Ogando, R. L. C., Paz-Chinch��n, F., Pereira, M. E. S., Malag��n, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Varga, T. N.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the combined results of eight searches for strong gravitational lens systems in the full 5,000 sq. deg. of Dark Energy Survey (DES) observations. The observations accumulated by the end of the third observing season fully covered the DES footprint in 5 filters (grizY), with an $i-$band limiting magnitude (at $10\sigma$) of 23.44. In four searches, a list of potential candidates was identified using a color and magnitude selection from the object catalogs created from the first three observing seasons. Three other searches were conducted at the locations of previously identified galaxy clusters. Cutout images of potential candidates were then visually scanned using an object viewer. An additional set of candidates came from a data-quality check of a subset of the color-coadd "tiles" created from the full DES six-season data set. A short list of the most promising strong lens candidates was then numerically ranked according to whether or not we judged them to be bona fide strong gravitational lens systems. These searches discovered a diverse set of 247 strong lens candidate systems, of which 81 are identified for the first time. We provide the coordinates, magnitudes, and photometric properties of the lens and source objects, and an estimate of the Einstein radius for 81 new systems and 166 previously reported. This catalog will be of use for selecting interesting systems for detailed follow-up, studies of galaxy cluster and group mass profiles, as well as a training/validation set for automated strong lens searches., Comment: 38 pages, 17 figures, 4 tables, accepted by ApJS
Published: 2021

36. Cross-correlation of DES Y3 lensing and ACT/${\it Planck}$ thermal Sunyaev Zel'dovich Effect II: Modeling and constraints on halo pressure profiles

Author: Pandey, S., Gatti, M., Baxter, E., Hill, J. C., Fang, X., Doux, C., Giannini, G., Raveri, M., DeRose, J., Huang, H., Moser, E., Battaglia, N., Alarcon, A., Amon, A., Becker, M., Campos, A., Chang, C., Chen, R., Choi, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Harrison, I., Maccrann, N., Mccullough, J., Myles, J., Alsina, A. Navarro, Prat, J., Rollins, R. P., Sanchez, C., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Bernstein, G. M., Bertin, E., Bolliet, B., Bond, J. R., Brooks, D., Calabrese, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Dunkley, J., Evrard, A. E., Ferraro, S., Ferrero, I., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Herner, K., Hincks, A. D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, J. P., Huterer, D., Jain, B., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Lahav, O., Lima, M., Lokken, M., Madhavacheril, M. S., Maia, M. A. G., Mcmahon, J. J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Nati, F., Niemack, M. D., Page, L., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schaan, E., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Spergel, D., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Wollack, E. J., and Xu, Z.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev Zel'dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe, and is sensitive to effects such as baryonic feedback. In a companion paper (Gatti et al. 2021), we present tomographic measurements and validation tests of the cross-correlation between galaxy shear measurements from the first three years of observations of the Dark Energy Survey, and tSZ measurements from a combination of Atacama Cosmology Telescope and ${\it Planck}$ observations. In this work, we use the same measurements to constrain models for the pressure profiles of halos across a wide range of halo mass and redshift. We find evidence for reduced pressure in low mass halos, consistent with predictions for the effects of feedback from active galactic nuclei. We infer the hydrostatic mass bias ($B \equiv M_{500c}/M_{\rm SZ}$) from our measurements, finding $B = 1.8\pm0.1$ when adopting the ${\it Planck}$-preferred cosmological parameters. We additionally find that our measurements are consistent with a non-zero redshift evolution of $B$, with the correct sign and sufficient magnitude to explain the mass bias necessary to reconcile cluster count measurements with the ${\it Planck}$-preferred cosmology. Our analysis introduces a model for the impact of intrinsic alignments (IA) of galaxy shapes on the shear-tSZ correlation. We show that IA can have a significant impact on these correlations at current noise levels., 22 pages, 13 figures. Comments welcome
Published: 2021

37. Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis

Author: Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Rosell, A. Carnero, Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespí, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., De Vicente, J., Mena-Fernández, J., Ross, A. J., Cid, D. Sanchez, Ferté, A., Brandao-Souza, A., Fang, X., Krause, E., Gomes, D., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Kind, M. Carrasco, Castander, F. J., Cawthon, R., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Percival, W. J., Malagón, A. A. Plazas, Rodriguez-Monroy, M., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Carnero Rosell, A., Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespi, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., De Vicente, J., Mena-Fernandez, J., Ross, A. J., Sanchez Cid, D., Ferte, A., Brandao-Souza, A., Fang, X., Krause, E., Gomes, D., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Carrasco Kind, M., Castander, F. J., Cawthon, R., Choi, A., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Percival, W. J., Plazas Malagon, A. A., Rodriguez-Monroy, M., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), The Ohio State University, Max-Planck-Institut für Astrophysik, Instituto de Astrofisica de Canarias, Laboratório Interinstitucional de e-Astronomia - LIneA, Dpto. Astrofísica, Universidad Autonoma de Madrid, University of Portsmouth, Sun Yat-sen University, Universidade Estadual Paulista (UNESP), ICTP South American Institute for Fundamental Research, Medioambientales y Tecnológicas (CIEMAT), Port d'Informació Científica (PIC), The Barcelona Institute of Science and Technology, California Institute of Technology, Universidade Estadual de Campinas (UNICAMP), University of Arizona, Universidade de São Paulo (USP), Rua General José Cristino, Fermi National Accelerator Laboratory, Institut d'Astrophysique de Paris, University College London, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, University of Wisconsin-Madison, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, University of Chicago, Santa Cruz Institute for Particle Physics, Stanford University, SLAC National Accelerator Laboratory, University of Queensland, Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, University of Waterloo, Perimeter Institute for Theoretical Physics, Princeton University, University of Southampton, Oak Ridge National Laboratory, Giessenbachstrasse, and Ludwig-Maximilians Universität München
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Halo occupation distribution, Galaxies: distances and redshifts, Observational cosmology, distances and redshifts [Galaxies], halo [Galaxy], Catalogs, Galaxy: halo, Methods: numerical, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, numerical [Methods], Computer Science::Information Retrieval, distances and redshift [Galaxies], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Redshift survey, Redshift, Galaxy, Space and Planetary Science, Dark energy, Catalog, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Ferrero, I., et al. (DES Collaboration), The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.
Published: 2021
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38. Shadows in the Dark: Low-Surface-Brightness Galaxies Discovered in the Dark Energy Survey

Author: Tanoglidis, D., Drlica-Wagner, A., Wei, K., Li, T. S., Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., DeRose, J., Conselice, C., Gagnon, L., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), UAM. Departamento de Física Teórica, Tanoglidis, D., Drlica-Wagner, A., Wei, K., T. S., Li, Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., Derose, J., Conselice, C., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, Sky surveys, 01 natural sciences, Imaging data, Luminosity, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Coma Cluster, Surface brightness, Sky survey, Global Air Sampling Program, education, 010303 astronomy & astrophysics, STFC, Low surface brightness galaxie, Physics, education.field_of_study, 010308 nuclear & particles physics, Física, RCUK, Astronomy and Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Star Formation, Dark energy, Low surface brightness galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a catalog of 23,790 extended low-surface-brightness galaxies (LSBGs) identified in $\sim 5000 ��^2$ from the first three years of imaging data from the Dark Energy Survey (DES). Based on a single-component S��rsic model fit, we define extended LSBGs as galaxies with $g$-band effective radii $R_{eff}(g) > 2.5''$ and mean surface brightness $\bar��_{eff}(g) > 24.2 \,mag ��rcsec^{-2}$. We find that the distribution of LSBGs is strongly bimodal in $(g-r)$ vs.\ $(g-i$) color space. We divide our sample into red ($g-i \geq 0.60$) and blue ($g-i 1.5 \,kpc$ and central surface brighthness $��_0(g) > 24.0\, mag \,arcsec^{-2}$. The wide-area sample of LSBGs in DES can be used to test the role of environment on models of LSBG formation and evolution., 31 pages, 19 figures. Version accepted for publication in ApJS. Data products related to this work can be found in: https://des.ncsa.illinois.edu/releases/other/y3-lsbg
Published: 2020
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39. Milky Way Satellite Census -- II. Galaxy-Halo Connection Constraints Including the Impact of the Large Magellanic Cloud

Author: Nadler, E.O., Wechsler, R.H., Bechtol, K., Mao, Y.-Y., Green, G., Drlica-Wagner, A., McNanna, M., Mau, S., Pace, A.B., Simon, J.D., Kravtsov, A., Dodelson, S., Li, T.S., Riley, A.H., Wang, M.Y., Abbott, T.M.C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G.M., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L.N., De Vicente, J., Desai, S., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W.G., Hinton, S.R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A.A., Romer, A.K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T.N., Walker, A.R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Kavli Institute for Particle Astrophysics and Cosmology, National Aeronautics and Space Administration (US), Department of Energy (US), Ministerio de Ciencia e Innovación (España), Science and Technology Facilities Council (UK), University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Generalitat de Catalunya, Nadler, E. O., Wechsler, R. H., Bechtol, K., Mao, Y. -Y., Green, G., Drlica-Wagner, A., Mcnanna, M., Mau, S., Pace, A. B., Simon, J. D., Kravtsov, A., Dodelson, S., T. S., Li, Riley, A. H., Wang, M. Y., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T. N., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Virial theorem, Galactic halo, Galaxy abundances, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Milky Way dark matter halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The population of Milky Way (MW) satellites contains the faintest known galaxies and thus provides essential insight into galaxy formation and dark matter microphysics. Here we combine a model of the galaxy-halo connection with newly derived observational selection functions based on searches for satellites in photometric surveys over nearly the entire high Galactic latitude sky. In particular, we use cosmological zoom-in simulations of MW-like halos that include realistic Large Magellanic Cloud (LMC) analogs to fit the position-dependent MW satellite luminosity function. We report decisive evidence for the statistical impact of the LMC on the MW satellite population due to an estimated 6 ± 2 observed LMC-associated satellites, consistent with the number of LMC satellites inferred from Gaia proper-motion measurements, confirming the predictions of cold dark matter models for the existence of satellites within satellite halos. Moreover, we infer that the LMC fell into the MW within the last 2 Gyr at high confidence. Based on our detailed full-sky modeling, we find that the faintest observed satellites inhabit halos with peak virial masses below 3.2× 10 M· at 95% confidence, and we place the first robust constraints on the fraction of halos that host galaxies in this regime. We predict that the faintest detectable satellites occupy halos with peak virial masses above 10 M·, highlighting the potential for powerful galaxy formation and dark matter constraints from future dwarf galaxy searches., This research received support from the National Science Foundation (NSF) under grant No. NSF AST-1517422, grant No. NSF PHY17-48958 through the Kavli Institute for Theoretical Physics program “The Small-Scale Structure of Cold(?) Dark Matter,” and grant No. NSF DGE-1656518 through the NSF Graduate Research Fellowship received by E.O.N. Support for Y.-Y.M. was provided by the Pittsburgh Particle Physics, Astrophysics and Cosmology Center through the Samuel P. Langley PITT PACC Postdoctoral Fellowship and NASA through NASA Hubble Fellowship grant No. HST-HF2-51441.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Part of this work was performed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. This research made use of computational resources at SLAC National Accelerator Laboratory, a U.S. Department of Energy Office; the authors are thankful for the support of the SLAC computational team. This research made use of the Sherlock cluster at the Stanford Research Computing Center (SRCC); the authors are thankful for the support of the SRCC team. This research made use of https://arXiv.org and NASA’s Astrophysics Data System for bibliographic information. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the NSFʼs National Optical-Infrared Astronomy Laboratory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This work is based in part on observations at Cerro Tololo Inter-American Observatory, NSFʼs National Optical-Infrared Astronomy Laboratory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. The IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by the Fermi Research Alliance, LLC, under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2019
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40. DES Y3 results: Blending shear and redshift biases in image simulations

Author: MacCrann, N., Becker, M. R., McCullough, J., Amon, A., Gruen, D., Jarvis, M., Choi, A., Troxel, M. A., Sheldon, E., Yanny, B., Herner, K., Dodelson, S., Zuntz, J., Eckert, K., Rollins, R. P., Varga, T. N., Bernstein, G. M., Gruendl, R. A., Harrison, I., Hartley, W. G., Sevilla-Noarbe, I., Pieres, A., Bridle, S. L., Myles, J., Alarcon, A., Everett, S., S��nchez, C., Huff, E. M., Tarsitano, F., Gatti, M., Secco, L. F., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Ferrero, I., Fert��, A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Wilkinson, R. D., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: As the statistical power of galaxy weak lensing reaches percent level precision, large, realistic and robust simulations are required to calibrate observational systematics, especially given the increased importance of object blending as survey depths increase. To capture the coupled effects of blending in both shear and photometric redshift calibration, we define the effective redshift distribution for lensing, $n_{\gamma}(z)$, and describe how to estimate it using image simulations. We use an extensive suite of tailored image simulations to characterize the performance of the shear estimation pipeline applied to the Dark Energy Survey (DES) Year 3 dataset. We describe the multi-band, multi-epoch simulations, and demonstrate their high level of realism through comparisons to the real DES data. We isolate the effects that generate shear calibration biases by running variations on our fiducial simulation, and find that blending-related effects are the dominant contribution to the mean multiplicative bias of approximately $-2\%$. By generating simulations with input shear signals that vary with redshift, we calibrate biases in our estimation of the effective redshfit distribution, and demonstrate the importance of this approach when blending is present. We provide corrected effective redshift distributions that incorporate statistical and systematic uncertainties, ready for use in DES Year 3 weak lensing analyses., Comment: Submitted to MNRAS. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release. Version accepted by mnras
Published: 2021

41. Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies

Author: Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., Li, T. S., McNanna, M., Riley, A. H., Garc��a-Bellido, J., Mao, Y. -Y., Green, G., Burke, D. L., Peter, A., Jain, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Brooks, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.
Subjects: High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At $95\%$ confidence, we report limits on (i) the mass of thermal relic warm DM, $m_{\rm WDM} > 6.5\ \mathrm{keV}$ (free-streaming length, $\lambda_{\rm{fs}} \lesssim 10\,h^{-1}\ \mathrm{kpc}$), (ii) the velocity-independent DM-proton scattering cross section, $\sigma_{0} < 8.8\times 10^{-29}\ \mathrm{cm}^{2}$ for a $100\ \mathrm{MeV}$ DM particle mass (DM-proton coupling, $c_p \lesssim (0.3\ \mathrm{GeV})^{-2}$), and (iii) the mass of fuzzy DM, $m_{\phi}> 2.9 \times 10^{-21}\ \mathrm{eV}$ (de Broglie wavelength, $\lambda_{\rm{dB}} \lesssim 0.5\ \mathrm{kpc}$). These constraints are complementary to other observational and laboratory constraints on DM properties., Comment: 15 pages, 5 figures, 2 tables. Updated to published version
Published: 2020

42. DES Y1 results: Splitting growth and geometry to test $��$CDM

Author: Muir, J., Baxter, E., Miranda, V., Doux, C., Fert��, A., Leonard, C. D., Huterer, D., Jain, B., Lemos, P., Raveri, M., Nadathur, S., Campos, A., Chen, A., Dodelson, S., Elvin-Poole, J., Lee, S., Secco, L. F., Troxel, M. A., Weaverdyck, N., Zuntz, J., Brout, D., Choi, A., Crocce, M., Davis, T. M., Gruen, D., Krause, E., Lidman, C., MacCrann, N., M��ller, A., Prat, J., Ross, A. J., Sako, M., Samuroff, S., S��chez, C., Scolnic, D., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., Garc��a-Bellido, J., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We analyze Dark Energy Survey (DES) data to constrain a cosmological model where a subset of parameters -- focusing on $��_m$ -- are split into versions associated with structure growth (e.g. $��_m^{\rm grow}$) and expansion history (e.g. $��_m^{\rm geo}$). Once the parameters have been specified for the $��$CDM cosmological model, which includes general relativity as a theory of gravity, it uniquely predicts the evolution of both geometry (distances) and the growth of structure over cosmic time. Any inconsistency between measurements of geometry and growth could therefore indicate a breakdown of that model. Our growth-geometry split approach therefore serves as both a (largely) model-independent test for beyond-$��$CDM physics, and as a means to characterize how DES observables provide cosmological information. We analyze the same multi-probe DES data as arXiv:1811.02375 : DES Year 1 (Y1) galaxy clustering and weak lensing, which are sensitive to both growth and geometry, as well as Y1 BAO and Y3 supernovae, which probe geometry. We additionally include external geometric information from BOSS DR12 BAO and a compressed Planck 2015 likelihood, and external growth information from BOSS DR12 RSD. We find no significant disagreement with $��_m^{\rm grow}=��_m^{\rm geo}$. When DES and external data are analyzed separately, degeneracies with neutrino mass and intrinsic alignments limit our ability to measure $��_m^{\rm grow}$, but combining DES with external data allows us to constrain both growth and geometric quantities. We also consider a parameterization where we split both $��_m$ and $w$, but find that even our most constraining data combination is unable to separately constrain $��_m^{\rm grow}$ and $w^{\rm grow}$. Relative to $��$CDM, splitting growth and geometry weakens bounds on $��_8$ but does not alter constraints on $h$., 35 pages, 18 figures. Updated to match published version
Published: 2020
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43. The Atacama Cosmology Telescope: A Catalog of > 4000 Sunyaev-Zel'dovich Galaxy Clusters

Author: Hilton, M., Sif��n, C., Naess, S., Madhavacheril, M., Oguri, M., Rozo, E., Rykoff, E., Abbott, T. M. C., Adhikari, S., Aguena, M., Aiola, S., Allam, S., Amodeo, S., Amon, A., Annis, J., Ansarinejad, B., Aros-Bunster, C., Austermann, J. E., Avila, S., Bacon, D., Battaglia, N., Beall, J. A., Becker, D. T., Bernstein, G. M., Bertin, E., Bhandarkar, T., Bhargava, S., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Carretero, J., Choi, S. K., Choi, A., Conselice, C., da Costa, L. N., Costanzi, M., Crichton, D., Crowley, K. T., D��nner, R., Denison, E. V., Devlin, M. J., Dicker, S. R., Diehl, H. T., Dietrich, J. P., Doel, P., Duff, S. M., Duivenvoorden, A. J., Dunkley, J., Everett, S., Ferraro, S., Ferrero, I., Fert��, A., Flaugher, B., Frieman, J., Gallardo, P. A., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giles, P., Golec, J. E., Gralla, M. B., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Han, D., Hartley, W. G., Hasselfield, M., Hill, J. C., Hilton, G. C., Hincks, A. D., Hinton, S. R., Ho, S-P. P., Honscheid, K., Hoyle, B., Hubmayr, J., Huffenberger, K. M., Hughes, J. P., Jaelani, A. T., Jain, B., James, D. J., Jeltema, T., Kent, S., Kind, M. Carrasco, Knowles, K., Koopman, B. J., Kuehn, K., Lahav, O., Lima, M., Lin, Y-T., Lokken, M., Loubser, S. I., MacCrann, N., Maia, M. A. G., Marriage, T. A., Martin, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Miyatake, H., Moodley, K., Morgan, R., Mroczkowski, T., Nati, F., Newburgh, L. B., Niemack, M. D., Nishizawa, A. J., Ogando, R. L. C., Orlowski-Scherer, J., Page, L. A., Palmese, A., Partridge, B., Paz-Chinch��n, F., Phakathi, P., Plazas, A. A., Robertson, N. C., Romer, A. K., Rosell, A. Carnero, Salatino, M., Sanchez, E., Schaan, E., Schillaci, A., Sehgal, N., Serrano, S., Shin, T., Simon, S. M., Smith, M., Soares-Santos, M., Spergel, D. N., Staggs, S. T., Storer, E. R., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Trac, H., Ullom, J. N., Vale, L. R., Van Lanen, J., Vavagiakis, E. M., De Vicente, J., Wilkinson, R. D., Wollack, E. J., Xu, Z., and Zhang, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences
Abstract: We present a catalog of 4195 optically confirmed Sunyaev-Zel'dovich (SZ) selected galaxy clusters detected with signal-to-noise > 4 in 13,211 deg$^2$ of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multi-frequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008-2018, and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ-signal vs. mass scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 x 10$^{14}$ MSun, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio > 5 in maps filtered at an angular scale of 2.4'. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ-signal mass-scaling relation, such as the Dark Energy Survey (4566 deg$^2$), the Hyper Suprime-Cam Subaru Strategic Program (469 deg$^2$), and the Kilo Degree Survey (825 deg$^2$). We highlight some noteworthy objects in the sample, including potentially projected systems; clusters with strong lensing features; clusters with active central galaxies or star formation; and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses, and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr., 35 pages, 27 figures, accepted for publication in ApJS; v1.0 catalogs will be available from LAMBDA https://lambda.gsfc.nasa.gov/product/act/actpol_prod_table.cfm; v1.0 catalogs available from https://astro.ukzn.ac.za/~mjh/ACTDR5/v1.0/ until then
Published: 2020
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44. $��_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses

Author: Pereira, M. E. S., Palmese, A., Varga, T. N., McClintock, T., Soares-Santos, M., Burgad, J., Annis, J., Farahi, A., Lin, H., Choi, A., DeRose, J., Esteves, J., Gatti, M., Gruen, D., Hartley, W. G., Hoyle, B., Jeltema, T., MacCrann, N., Roodman, A., S��nchez, C., Shin, T., von der Linden, A., Zuntz, J., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Wechsler, R. H., Weller, J., and Zhang, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the weak lensing mass calibration of the stellar mass based $��_{\star}$ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time we are able to perform a calibration of $��_{\star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z, 20 pages, 10 figures, submitted to MNRAS
Published: 2020
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45. Dark Energy Survey year 1 results: constraints on extended cosmological models from galaxy clustering and weak lensing

Author: DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Avila, S., Banerji, M., Baxter, E., Bechtol, K., Becker, M. R., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Evrard, A. E., Fernandez, E., Fert��, A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Lemos, P., Leonard, C. D., Li, T. S., Liddle, A. R., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Nichol, R. C., Nord, B., Ogando, R. L. C., Plazas, A. A., Raveri, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Samuroff, S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vikram, V., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Zhang, Y., Zuntz, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, UAM. Departamento de Física Teórica, Natl Opt Astron Observ, UCL, Rhodes Univ, Univ Portsmouth, Univ Cambridge, Univ Penn, LSST, Argonne Natl Lab, Inst Astrophys Paris, UPMC Univ Paris 06, Ohio State Univ, Ecole Polytech Fed Lausanne, Univ Manchester, Stanford Univ, SLAC Natl Accelerator Lab, Universidade Estadual Paulista (Unesp), Carnegie Mellon Univ, Lab Interinst & Astron LIneA, Observ Nacl, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, CSIC, IEEC, Univ Chicago, Univ Michigan, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Fermilab Natl Accelerator Lab, Excellence Cluster Universe, Ludwig Maximilians Univ Munchen, CALTECH, Steward Observ, Univ Edinburgh, Univ Autonoma Madrid, Swiss Fed Inst Technol, Santa Cruz Inst Particle Phys, Max Planck Inst Extraterr Phys, Lawrence Berkeley Natl Lab, Australian Astron Observ, Universidade de São Paulo (USP), Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Univ Sussex, Univ Southampton, Brandeis Univ, Universidade Estadual de Campinas (UNICAMP), Oak Ridge Natl Lab, National Optical Astronomy Observatory, University College London, Rhodes University, University of Portsmouth, University of Cambridge, University of Pennsylvania, Argonne National Laboratory, Institut d'Astrophysique de Paris, Ohio State University, Observatoire de Sauverny, University of Manchester, Stanford University, SLAC National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Carnegie Mellon University, Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, Institute of Space Sciences (ICE-CSIC), Institut d'Estudis Espacials de Catalunya (IEEC), University of Chicago, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), 382 Via Pueblo Mall, Fermi National Accelerator Laboratory, Ludwig-Maximilians-Universität, California Institute of Technology, University of Edinburgh, Oak Ridge National Laboratory, Universidad Autonoma de Madrid, Ludwig-Maximilians Universität München, ETH Zurich, Santa Cruz Institute for Particle Physics, Max Planck Institute for Extraterrestrial Physics, Lawrence Berkeley National Laboratory, Australian Astronomical Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Sussex, University of Southampton, and Physics Department
Subjects: luminous red galaxies, Planck, cosmological model, geometry, MATÉRIA ESCURA, gravitation: model, Cosmic microwave background, Astrophysics, cosmic background radiation, 4/3, des, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), redshift distributions, Weak gravitational lensing, Physics, nucleosynthesis, neutrinos, hep-ph, High Energy Physics - Phenomenology, curvature, astro-ph.CO, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], lambda, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, gr-qc, Dark matter, equation of state: time dependence, sloan digital sky survey, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), dark matter, efficient, symbols.namesake, gravitation: lens, 0103 physical sciences, 010306 general physics, STFC, 010308 nuclear & particles physics, Física, RCUK, redshift, Redshift, gravity, Automatic Keywords, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, dark energy: equation of state
Abstract: We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, $\Lambda$CDM and $w$CDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: 1) nonzero curvature $\Omega_k$, 2) number of relativistic species $N_{\rm eff}$ different from the standard value of 3.046, 3) time-varying equation-of-state of dark energy described by the parameters $w_0$ and $w_a$ (alternatively quoted by the values at the pivot redshift, $w_p$, and $w_a$), and 4) modified gravity described by the parameters $\mu_0$ and $\Sigma_0$ that modify the metric potentials. We also consider external information from Planck CMB measurements; BAO measurements from SDSS, 6dF, and BOSS; RSD measurements from BOSS; and SNIa information from the Pantheon compilation. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find $\Omega_k=0.0020^{+0.0037}_{-0.0032}$ at the 68% confidence level, and $N_{\rm eff}, Comment: 22 pages, 7 figures, matches the published version
Published: 2019
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46. Dark Energy Survey year 1 results: Joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions

Author: Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E. J., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bleem, L. E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chang, C. L., Cho, H-M., Choi, A., Chown, R., Crawford, T. M., Crites, A. T., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., de Haan, T., DeRose, J., Desai, S., De Vicente, J., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Everett, W. B., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Garc��a-Bellido, J., Gatti, M., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Knox, L., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Lin, H., Luong-Van, D., MacCrann, N., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Muir, J., Natoli, T., Nicola, A., Nord, B., Omori, Y., Padin, S., Pandey, S., Plazas, A. A., Porredon, A., Prat, J., Pryke, C., Rau, M. M., Reichardt, C. L., Rollins, R. P., Romer, A. K., Roodman, A., Ross, A. J., Rozo, E., Ruhl, J. E., Rykoff, E. S., Samuroff, S., S��nchez, C., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vanderlinde, K., Vieira, J. D., Vielzeuf, P., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Williamson, R., Wu, W. L. K., Yanny, B., Zahn, O., Zhang, Y., Zuntz, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, and SPT
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, FOS: Physical sciences, Context (language use), Field (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Omega, Galaxy, Cosmology, South Pole Telescope, 0103 physical sciences, Dark energy, astro-ph.CO, LENTES GRAVITACIONAIS, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev-Zel'dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat $\Lambda$CDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields $S_{8}\equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3} = 0.782^{+0.019}_{-0.025}$ and $\Omega_{\rm m}=0.260^{+0.029}_{-0.019}$. We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat $\Lambda$CDM models. Combining constraints from all six two-point functions yields $S_{8}=0.776^{+0.014}_{-0.021}$ and $\Omega_{\rm m}= 0.271^{+0.022}_{-0.016}$. These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis., Comment: 20 pages, 7 figures
Published: 2019
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47. First Cosmology Results Using Type Ia Supernovae From the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

Author: Brout, D., Scolnic, D., Kessler, R., D'Andrea, C. B., Davis, T. M., Gupta, R. R., Hinton, S. R., Kim, A. G., Lasker, J., Lidman, C., Macaulay, E., M��ller, A., Nichol, R. C., Sako, M., Smith, M., Sullivan, M., Zhang, B., Andersen, P., Asorey, J., Avelino, A., Bassett, B. A., Brown, P., Calcino, J., Carollo, D., Challis, P., Childress, M., Clocchiatti, A., Filippenko, A. V., Foley, R. J., Galbany, L., Glazebrook, K., Hoormann, J. K., Kasai, E., Kirshner, R. P., Kuehn, K., Kuhlmann, S., Lewis, G. F., Mandel, K. S., March, M., Miranda, V., Morganson, E., Muthukrishna, D., Nugent, P., Palmese, A., Pan, Y. -C., Sharp, R., Sommer, N. E., Swann, E., Thomas, R. C., Tucker, B. E., Uddin, S. A., Wester, W., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., Bechtol, K., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jarvis, M., Jeltema, T., Krause, E., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., Marriner, J., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Zhang, Y., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified type Ia supernovae (SNe Ia) from the first three years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017, Comment: 30 Pages, 18 Figures, 12 Tables. Submitted to ApJ. Comments welcome
Published: 2019
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48. First Cosmology Results Using Type Ia Supernovae From the Dark Energy Survey: Survey Overview and Supernova Spectroscopy

Author: D'Andrea, C. B., Smith, M., Sullivan, M., Nichol, R. C., Thomas, R. C., Kim, A. G., Möller, A., Sako, M., Castander, F. J., Filippenko, A. V., Foley, R. J., Galbany, L., González-Gaitán, S., Kasai, E., Kirshner, R. P., Lidman, C., Scolnic, D., Brout, D., Davis, T. M., Gupta, R. R., Hinton, S. R., Kessler, R., Lasker, J., Macaulay, E., Wolf, R. C., Zhang, B., Asorey, J., Avelino, A., Bassett, B. A., Calcino, J., Carollo, D., Casas, R., Challis, P., Childress, M., Clocchiatti, A., Crawford, S., Glazebrook, K., Goldstein, D. A., Graham, M. L., Hoormann, J. K., Kuehn, K., Lewis, G. F., Mandel, K. S., Morganson, E., Muthukrishna, D., Nugent, P., Pan, Y. -C., Pursiainen, M., Sharp, R., Sommer, N. E., Swann, E., Tucker, B. E., Uddin, S. A., Wiseman, P., Zheng, W., Abbott, T. M. C., Annis, J., Avila, S., Bechtol, K., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Eifler, T. F., Estrada, J., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Johnson, M. W. G., Johnson, M. D., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sobreira, F., Suchyta, E., Tarle, G., Tucker, D. L., Wester, W., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present spectroscopy from the first three seasons of the Dark Energy Survey Supernova Program (DES-SN). We describe the supernova spectroscopic program in full: strategy, observations, data reduction, and classification. We have spectroscopically confirmed 307 supernovae, including 251 type Ia supernovae (SNe Ia) over a redshift range of $0.017 < z < 0.85$. We determine the effective spectroscopic selection function for our sample, and use it to investigate the redshift-dependent bias on the distance moduli of SNe Ia we have classified. We also provide a full overview of the strategy, observations, and data products of DES-SN, which has discovered 12,015 likely supernovae during these first three seasons. The data presented here are used for the first cosmology analysis by DES-SN ('DES-SN3YR'), the results of which are given in DES Collaboration (2018a)., 25 pages, 14 figures, 8 tables. Submitted to AJ
Published: 2018

49. Dark Energy Survey Year 1 Results: Methods for Cluster Cosmology and Application to the SDSS

Author: Costanzi, M., Rozo, E., Simet, M., Zhang, Y., Evrard, A. E., Mantz, A., Rykoff, E. S., Jeltema, T., Gruen, D., McClintock, S. Allen T., Romer, A. K., von der Linden, A., Farahi, A., DeRose, J., Varga, T. N., Weller, J., Giles, P., Hollowood, D. L., Bhargava, S., Bermeo-Hernandez, A., Chen, X., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Wechsler, R. H.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform the first blind analysis of cluster abundance data. Specifically, we derive cosmological constraints from the abundance and weak-lensing signal of \redmapper\ clusters of richness $\lambda\geq 20$ in the redshift range $z\in[0.1,0.3]$ as measured in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness--mass relation of the clusters. For a flat $\Lambda$CDM cosmological model with massive neutrinos, we find $S_8 \equiv \sigma_{8}(\Omega_m/0.3)^{0.5}=0.79^{+0.05}_{-0.04}$. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES) and the Kilo-Degree Survey (KiDS), and with the Cosmic Microwave Background (CMB) anisotropies as measured by \planck. We demonstrate that the cosmological posteriors are robust against variation of the richness--mass relation model and to systematics associated with the calibration of the selection function. In combination with Baryon Acoustic Oscillation (BAO) data and Big-Bang Nucleosynthesis (BBN) data, we constrain the Hubble rate to be $h=0.66\pm 0.02$, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness--mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set., Comment: 25 pages, 14 figures
Published: 2018

50. Dark Energy Survey Year 1 Results: Cross-correlation between DES Y1 galaxy weak lensing and SPT+Planck CMB weak lensing

Author: Omori, Y., Baxter, E., Chang, C., Kirk, D., Alarcon, A., Bernstein, G. M., Bleem, L. E., Cawthon, R., Choi, A., Chown, R., Crawford, T. M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T. F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M. M., Reichardt, C. L., Rozo, E., Samuroff, S., S��nchez, C., Secco, L. F., Sheldon, E., Simard, G., Troxel, M. A., Vielzeuf, P., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Crocce, M., Cunha, C. E., da Costa, L. N., de Haan, T., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Fernandez, E., Flaugher, B., Frieman, J., Garc��a-Bellido, J., George, E. M., Gruendl, R. A., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hollowood, D. L., Honscheid, K., Holzapfel, W. L., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A. T., Leitch, E. M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Mocanu, L. M., Mohr, J. J., Natoli, T., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Scarpine, V., Schaffer, K. K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., Wu, W. L. K., and Zahn, O.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one (Y1) data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg$^{2}$. With the combined measurements from four source galaxy redshift bins, we reject the hypothesis of no lensing with a significance of $10.8\sigma$. When employing angular scale cuts, this significance is reduced to $6.8\sigma$, which remains the highest signal-to-noise measurement of its kind to date. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial $\Lambda$CDM model, finding $A = 0.99 \pm 0.17$. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the $\Lambda$CDM model, we obtain the marginalized constraints of $\Omega_{\rm m}=0.261^{+0.070}_{-0.051}$ and $S_{8}\equiv \sigma_{8}\sqrt{\Omega_{\rm m}/0.3} = 0.660^{+0.085}_{-0.100}$. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT and Planck data., Comment: 15 pages, 6 figures
Published: 2018

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